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2024 Journal of Geophysical Research Articles

Report generated on 02/04/2025 13:54:02

cdaweb was referenced in 105 papers
spdf was referenced in 67 papers
space physics data facility was referenced in 66 papers
omni was referenced in 160 papers
omni2 was referenced in 3 papers
omni-2 was referenced in 8 papers
omniweb was referenced in 142 papers
sscweb was referenced in 4 papers
iri was referenced in 37 papers
international reference ionosphere was referenced in 29 papers
vitmo was referenced in 2 papers
heliocloud was referenced in 1 papers
301 of 635 possible papers ( 47% ) contained references to SPDF keywords

Papers:

Authors=Vaishnav, Rajesh; Jacobi, Christoph; Berdermann, Jens; Schmolter, Erik; Duhnen, Hanna; Codrescu, Mihail;Title=Ionospheric Response to Solar EUV Radiation Variations Using GOLD Observations and the CTIPe Model, 2024, doi:10.1029/2022JA030887, ID:26803861.Keywords: omniwebSample usage ( BODY ) =We make use of the daily Kp indices from the OMNIWeb Plus database (NASA, 2022d) to describe geomagnetic activity.

Authors=Kepko, L.; Viall, N. M.; DiMatteo, S.;Title=Periodic Mesoscale Density Structures Comprise a Significant Fraction of the Solar Wind and Are Formed at the Sun, 2024, doi:10.1029/2023JA031403, ID:26803871.Keywords: cdaweb, space physics data facilitySample usageThe spectral analysis code of Di Matteo et al. ( 2021) that is used in this paper is freely available from Zenodo (Di Matteo et al., 2020).Sample usage ( BODY ) =Data Availability Statement All wind SWE data are available from the Space Physics Data Facility located at http://cdaweb.gsfc.nasa.gov (Ogilvie et al., 2021).

Authors=Greeley, A. D.; Kanekal, S. G.; Schiller, Q.; Blum, L.; Halford, A.; Murphy, K.; Raita, T.; Baker, D. N.;Title=Persistent Pitch Angle Anisotropies of Relativistic Electrons in the Outer Radiation Belts, 2024, doi:10.1029/2023JA03154910.22541/essoar.168167400.03912545/v1, ID:26803883.Keywords: spdf, space physics data facility, omniwebSample usage ( BODY ) =Van Allen Probes and OMNIWeb data can be found through NASA’s Space Physics Data Facility (SPDF) at https://spdf.gsfc.nasa.gov/. The authors thank T. Raita for data access, and more information on SGO data and overview plots can be found at https://www.sgo.fi/index.php. Sample usage ( BODY ) =Panels (e-g) show SymH, p density, and magnetic field components from OMNIWeb data. Time and MLAT are shown on the x -axis. 3 Figure Pitch angle index (PAI) summary plots for 27 June 2013.

Authors=Wong, Jin-Mann; Meredith, Nigel P.; Horne, Richard B.; Glauert, Sarah A.; Ross, Johnathan P. J.;Title=New Chorus Diffusion Coefficients for Radiation Belt Modeling, 2024, doi:10.1029/2023JA031607, ID:26803889.Keywords: omniwebSample usage ( ACK ) =We also acknowledge the Radiation Belt Storm Probes ECT Science Operations and Data Center for the provision of the magnetic ephemeris data, available online ( https://www.rbsp-ect.lanl.gov/data-pub/rbspa/MagEphem/ ). We thank the NSSDC Omniweb for the provision of the Kp indices used in this paper. The research leading to these results has received funding from the Natural Environment Research Council (NERC) Highlight Topic Grant NE/P01738X/1 (Rad-Sat) and the NERC Grants NE/V00249X/1 (Sat-Risk), NE/R016038/1, and NE/X000389/1.

Authors=Reidy, J. A.; Horne, R. B.; Glauert, S. A.; Clilverd, M. A.; Meredith, N. P.; Rodger, C. J.; Ross, J. P.; Wong, J.;Title=Characterizing Radiation-Belt Energetic Electron Precipitation Spectra: A Comparison of Quasi-Linear Diffusion Theory With In Situ Measurements, 2024, doi:10.1029/2023JA031641, ID:26803895.Keywords: omni, omniwebSample usage ( BODY ) =The Kp indices were downloaded from the OMNI database ( https://omniweb.gsfc.nasa.gov/ ). The Chorus wave pitch angle diffusion coefficients calculated for use in this study have been published in the Polar Data Centre ( https://doi.org/10.5285/5ef0d6cd-67c2-48fc-8a6a-dfe44a63979e ) (Reidy et al., 2023).

Authors=Engebretson, Mark J.; Yang, Lily; Steinmetz, Erik S.; Pilipenko, Vyacheslav A.; Moldwin, Mark B.; McCuen, Brett A.; Connors, Martin G.; Weygand, James M.; Waters, Colin L.; Nishimura, Yukitoshi; Lyons, Larry R.; Russell, Christopher T.;Title=Extreme Geomagnetic Disturbances (GMDs) Observed in Eastern Arctic Canada: Occurrence Characteristics and Solar Cycle Dependence, 2024, doi:10.1029/2023JA03164310.22541/essoar.168298702.26747467/v1, ID:26803901.Keywords: cdaweb, space physics data facility, omniSample usage ( BODY ) =Figure 2c shows yearly medians and 25th and 75th percentile values of the solar wind velocity (Vsw), based on 1-hr averages obtained from the OMNI database via CDAWEB ( https://cdaweb.gsfc.nasa.gov/ ) for these same years. The largest annual median and especially 75th percentile velocities coincided in time with the largest GMD occurrence percentages (2015-2017) and the smallest annual velocities (2013-2014 and 2020) coincided approximately with the smallest GMD occurrence percentages (2012-2014 and 2020). Sample usage ( BODY ) =OMNI data are available from the Coordinated Data Analysis Web (CDAWeb) part of the Space Physics Data Facility at the NASA Goddard Space Flight Center (Papitashvili King, 2020).

Authors=Sanchez-Garcia, E.; Gonzalez-Esparza, J. A.; Aguilar-Rodriguez, E.; Corona-Romero, P.;Title=Stream Interaction Regions in the Minimum of Solar Cycles 23 and 24, 2024, doi:10.1029/2023JA031685, ID:26803916.Keywords: omniwebSample usage ( BODY ) =The databases of Wind and DSCOVR are available on OMNIWeb (https://omniweb.gsfc.nasa.gov). We used the global indices Kp and Dst to quantify the intensity of the GS.

Authors=Salinas, Hector A.; Wilder, Frederick D.; Lopez, Ramon E.; Strangeway, Robert J.; Giles, Barbara L.; Burch, James L.; Torbert, Roy B.; Oka, Mitsuo;Title=Statistical Analysis of Electric Currents Within the Magnetosheath Using Dayside Magnetospheric Multiscale Mission Observations, 2024, doi:10.1029/2023JA031698, ID:26803921.Keywords: cdaweb, spdf, space physics data facility, omni, omniwebSample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s OMNIWeb (or CDAWeb or ftp) service, and OMNI data. This research was supported by NASA Grant 80NSSC21K0492 and NASA’s MMS mission. Sample usage ( ACK ) =MMS data is also publicly accessible at the Space Physics Data Facility (SPDF) at the NASA Goddard Space Flight Center (https://spdf.gsfc.nasa.gov/pub/data/mms/).

Authors=Chen, Yun-Ju; Heelis, Roderick; Hairston, Marc; Valladares, Cesar;Title=The Hemispheric Difference in Electric Potential and Electron Precipitation Observed by DMSP in the Auroral Zone, 2024, doi:10.1029/2023JA031733, ID:26803926.Keywords: cdaweb, spdf, space physics data facility, omniwebSample usage ( BODY ) =The DMSP particle and magnetic field data are obtained at NASA SPDF CDAWeb contributed from the staff at AFRL, NGDC and CU ( http://cdaweb.gsfc.nasa.gov/istp_public/ ). To access the DMSP particle and magnetic field data, go to “cdaweb.gsfc.nasa.gov/istp_public/” and select “DMSP.” A list of “DMSP-Fxx_SSJ_PRECIPITATING-ELECTRONS-IONS” and “DMSP-Fxx_SSM_ MAGNETOMETER” will be produced. After selecting the desired data products, the “CDAWeb Data Explorer” page will appear, where data and information about the data are available to review and download. Sample usage ( BODY ) =These data are available via the Space Physics Data Facility OMNIWeb interface and are propagated in time to correspond to the time at the Earth’s bow shock.

Authors=Cai, Xuguang; Wang, Wenbin; Eastes, Richard W.; Qian, Liying; Correira, J.; McClintock, William E.;Title=Investigation of Different SO/N2 Variations Observed by GOLD During a Minor Geomagnetic Storm From 2 to 4 August 2021, 2024, doi:10.1029/2023JA031782, ID:26803940.Keywords: cdaweb, omniwebSample usage ( BODY ) =Data Availability Statement The IMF and solar wind data is from https://cdaweb.gsfc.nasa.gov/cgi-bin/eval1.cgi . The F10.7, Kp and Dst are from https://omniweb.gsfc.nasa.gov/form/dx1.html. The GOLD SO/N 2 and Q EUV are from https://gold.cs.ucf.edu/data/search/ .

Authors=Wei, Lehui; Jiang, Chunhua; Yokoyama, Tatsuhiro; Liu, Jing; Yang, Guobin; Hu, Yaogai;Title=Investigation of the Occurrence Characteristics and Possible Origins of Daytime Spread F Irregularities in Low Latitude Region, 2024, doi:10.1029/2023JA031809, ID:26803953.Keywords: spdf, omniwebSample usage ( ACK ) =We acknowledge the use of the open data from SPDF, NASA, USA. The authors sincerely appreciate the patience and the helpful comments of the reviewers. Sample usage ( BODY ) =Data Availability Statement The 3h Kp index and F 10.7 solar flux through SPDF, NASA, USA ( https://omniweb.gsfc.nasa.gov/ ). Geomagnetic latitudes were calculated by IGRF-12 in this study.

Authors=Fowler, C. M.; Shaver, S.; Hanley, K. G.; Andersson, L.; McFadden, J.; Mitchell, D.; Halekas, J.; Ma, Y.; Espley, J.; Curry, S.;Title=Disappearing Solar Wind at Mars: Changes in the Mars-Solar Wind Interaction, 2024, doi:10.1029/2023JA031910, ID:26803966.Keywords: omniSample usage ( BODY ) =(a): magnetic field magnitude (black) with the Morschhauser spherical harmonic crustal magnetic field model (Morschhauser et al., 2014) (orange); (b): magnetic field vector; (c): angle the magnetic field makes relative to the local zenith direction; (d): SWIA omni-directional ion energy flux; (e), (f): STATIC omni-directional ion energy flux and mass spectra. The green line in panel (e) marks the (negative of) spacecraft potential as measured by STATIC; (g): SWEA omni-directional suprathermal electron energy spectrum; (h): LPW I-V sweeps.

Authors=Kato, Yuto; Shiokawa, Kazuo; Tanaka, Yoshimasa; Ozaki, Mitsunori; Kadokura, Akira; Oyama, Shin-ichiro; Oinats, Alexey; Connors, Martin; Baishev, Dmitry;Title=Longitudinal Development of Cosmic Noise Absorption Based on Multipoint Observations at Subauroral Latitudes During Storm-Time Substorms on 25-28 August 2018, 2024, doi:10.1029/2023JA031950, ID:26803972.Keywords: cdaweb, space physics data facility, omni, omniwebSample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s OMNIWeb (or CDAWeb or ftp) service, and OMNI data (King and Papitashvili ( 2005); Papitashvili and King ( 2020)). The Wp index used in this paper was provided by the World Data Center for Geomagnetism, Kyoto. Sample usage ( BODY ) =To examine the CNA in relation to interplanetary space parameters, we also used IMF and solar wind parameters provided by the OMNIWeb ( http://omniweb.gsfc.na-sa.gov/form/omni_min.html; King and Papitashvili ( 2005); Papitashvili and King ( 2020)).

Authors=Liu, Xiaocan; Han, Peng; Hattori, Katsumi; Chen, Huaran; Chen, Junjie; Jiao, Liguo; Tu, Jiyao; Lei, Yu; Zhao, Junhao;Title=Seasonal Variations of Sq Current System in Different Longitudinal Sectors and Solar Activities, 2024, doi:10.1029/2023JA031956, ID:26803984.Keywords: cdawebSample usage ( BODY ) =The sunspot number and solar flux F 10.7 index are downloaded from NASA (check box of Activity Indices in https://cdaweb.gsfc.nasa.gov/ ).

Authors=Park, Jaeheung;Title=Climatology of Martian Ionospheric Disturbances Deduced From MAVEN Data in 2014-2023, 2024, doi:10.1029/2023JA031991, ID:26803993.Keywords: cdaweb, omniwebSample usage ( BODY ) =Data Availability Statement The MAVEN data used for this study are available at the NASA-CDAWeb ( https://cdaweb.gsfc.nasa.gov/pub/data/maven/insitu/kp-4sec/cdfs/ ).Sample usage ( BODY ) =To test this conjecture, we calculate daily averages of (unfiltered) solar wind (SW) electron density and temperature observed by MAVEN, by analogy with daily averaged near-Earth SW parameters provided by OMNIWeb of the National Aeronautics and Space Administration (NASA). Specifically, we use the ” SWEA_Electron_density ” and ” SWEA_Electron_temperature ” in the MAVEN/KP4SEC files for daily averages and impose no additional restriction on the observation heights.

Authors=Franz, M.; Rojo, M.; Cornet, T.; Hadid, L. Z.; Saito, Y.; Andre, N.; Varsani, A.; Schmid, D.; Kruger, H.; Krupp, N.; Delcourt, D.; Katra, B.; Harada, Y.; Yokota, S.; Verdeil, C.; Aizawa, S.; Millilo, A.; Orsini, S.; Mangano, V.; Fiethe, B.; Benkhoff, J.; Murakami, G.;Title=Spacecraft Outgassing Observed by the BepiColombo Ion Spectrometers, 2024, doi:10.1029/2023JA032044, ID:26803999.Keywords: omniSample usage ( BODY ) =The field of view is adjustable from 6.4deg x 270deg-9.6deg x 270deg with respective geometric factors of 1.23 x 10 -5 and 4.64 x 10 -4 cm 2 -sr-eV/eV for the products used in this study. These are the omni-directional energy spectra (“Et”) which are divided into 4 sectors “d1” to “d4” with 128 energy steps in solar wind mode at time resolution of 16 s.

Authors=Wang, Hui; Luhr, Hermann;Title=IMF By Effects on the Strength and Latitude of Polar Electrojets: CHAMP and Swarm Joint Observations, 2024, doi:10.1029/2023JA032049, ID:26804002.Keywords: space physics data facility, omniwebSample usage ( BODY ) =The solar wind and interplanetary magnetic field and magnetic activity index data are from NASA/GSFC’S Space Physics Data Facility’s OMNIWeb ( https://omniweb.gsfc.nasa.gov ).Authors=Gao, Zhonglei; Zhou, Yaxiong; Yang, Hongming; Liu, Si; Xiao, Fuliang; Yang, Chang; He, Yihua; Zhou, Qinghua;Title=A Statistical Study of Quasi-Electrostatic Magnetosonic Waves, 2024, doi:10.1029/2023JA032064, ID:26804005.Keywords: spdfSample usage ( BODY ) =Data Availability Statement Van Allen Probes data for this research are available at the website https://spdf.gsfc.nasa.gov/pub/data/rbsp/ . The file recording the time periods of QEMS waves is available at (Gao, 2023).

Authors=Gao, Hong; Xu, Jiyao; Chen, Guang-Ming; Zhu, Yajun; He, Maosheng; Yuan, Wei; Sun, Longchang; Li, Dan; Liu, Hongshan;Title=Response of ICON/MIGHTI Measured Low-Mid Latitude OI630.0 and OI557.7 nm Dayglow Emissions to the 27 August 2021 Geomagnetic Storm, 2024, doi:10.1029/2023JA032070, ID:26804009.Keywords: spdf, space physics data facility, omni, omni2, omni-2Sample usage ( ACK ) =ICON data are processed in the ICON Science Data Center at UCB (University of California, Berkeley) ( https://icon.ssl.berkeley.edu/Data ) and archived at the NASA (National Aeronautics and Space Administration) Space Physics Data Facility ( https://spdf.gsfc.nasa.gov/ ).Sample usage ( BODY ) =Reported hourly data of the geomagnetic Dst index and daily data of the F10.7 Solar Radio Flux are OMNI2 data, which are available at https://spdf.gsfc.nasa.gov/pub/data/omni/.

Authors=Xiong, Senlin; Dai, Lei; Wang, Chi; Yang, Xiaochao; Wygant, John R.; Baker, Daniel N.;Title=Rapid Relativistic Electron Enhancements and Associated Particle Injections: A Multi-Spacecraft Statistical Study, 2024, doi:10.1029/2023JA032095, ID:26804022.Keywords: cdaweb, spdf, omni, omniwebSample usage ( BODY ) =Data Availability Statement The RBSP data and ACE data are available at GSFC/SPDF ( https://cdaweb.gsfc.nasa.gov/pub/data/rbsp/ , https://cdaweb.gsfc.nasa.gov/pub/data/ace/ ). Sample usage ( BODY ) =AE-AL index and SYM-H index are from the OMNI database. The solar wind plasma and magnetic field data from the Advance Composition Explorer (ACE) spacecraft, are adopted to diagnose the type of geomagnetic storms. Sample usage ( BODY ) =Geomagnetic index data is available at https://omniweb.gsfc.nasa.gov/ .

Authors=Adhitya, P.; Bulusu, Jayashree; Sinha, A. K.; Vichare, Geeta;Title=Examining the Applicability of Direct Analytic Method (DAM) to Normal Modes of Poloidal Oscillations Under Symmetric and Asymmetric Boundary Conditions, 2024, doi:10.1029/2023JA032119, ID:26804041.Keywords: cdaweb, spdf, space physics data facility, iriSample usage ( BODY ) =The satellite data of Van Allen Probes satellite is obtained from Space Physics Data Facility (SPDF), GSFC ( https://cdaweb.gsfc.nasa.gov/ ). For the calculation of R , the data of ionospheric conductivities is obtained from Ionospheric conductivity model on WDC Kyoto ( https://wdc.kugi.kyoto-u.ac.jp/ionocond/sigcal/index.html ) and ion composition is obtained from IRI-16 model ( https://kauai.ccmc.gsfc.nasa.gov/instantrun/**iri**/ ) (Bilitza, 1990; Rees, 1988).Sample usage ( ACK ) =The open data policy of Space Physics Data Facility (SPDF), GSFC and WDC Kyoto is duly acknowledged. For the calculation of R , the data of ionospheric conductivities is obtained from Ionospheric conductivity model on WDC Kyoto ( https://wdc.kugi.kyoto-u.ac.jp/ionocond/sigcal/index.html ) and ion composition is obtained from IRI-16 model ( https://kauai.ccmc.gsfc.nasa.gov/instantrun/**iri**/ ) (Bilitza, 1990; Rees, 1988).Sample usage ( BODY ) =The model can be extended to lower L -values by taking proper composition of ion percentage of different species through working models such as IRI-2016. Field Aligned Structural Variation of Poloidal Half Wave Field line structures of latitudinal variation of electric field and magnetic field are obtained analytically using DAM model and numerically by using NES model.

Authors=Wei, Jiayun; Zou, Zhengyang; Zuo, Pingbing; Ni, Binbin; Ruan, Mengsi; Feng, Xueshang;Title=Commencement and Interruption of Relativistic Electron Dropout in the Heart of the Outer Radiation Belt Induced by a Magnetic Cloud Event, 2024, doi:10.1029/2023JA032138, ID:26804051.Keywords: cdaweb, spdf, omni, omniwebSample usage ( BODY ) =Data Availability Statement The Wind MFI and SWE data and geomagnetic indices are available at NASA OmniWeb ( http://cdaweb.gsfc.nasa.gov ). The REPT and MagEIS data are obtained from https://spdf.gsfc.nasa.gov/pub/data/rbsp. Sample usage ( BODY ) =The REPT and MagEIS data are obtained from https://spdf.gsfc.nasa.gov/pub/data/rbsp. The EMFISIS data are derived from https://emfisis.physics.uiowa.edu/data/index . Sample usage ( BODY ) =In addition, the geomagnetic indices (e.g., SymH and AE) at a 1-min resolution obtained from the OMNI database, the magnetic field data from the Magnetic Field Investigation (MFI) (Lepping et al., 1995) and plasma data from the Solar Wind Experiment (SWE) (Ogilvie et al., 1995) on board the WIND spacecraft to identify solar wind disturbances.

Authors=Denton, Richard E.; Liu, Yi-Hsin; Agudelo Rueda, Jefferson A.; Genestreti, Kevin J.; Hasegawa, Hiroshi; Hosner, Martin; Torbert, Roy B.; Burch, James L.;Title=Determining the Orientation of a Magnetic Reconnection X Line and Implications for a 2D Coordinate System, 2024, doi:10.1029/2023JA032167, ID:26804057.Keywords: omniwebSample usage ( BODY ) =But in that case, the magnetic field on both sides of the current sheet was far from steady, and plots of solar wind quantities from OmniWeb (King Papitashvili, 2005) showed that there were dramatic changes in the solar wind quantities corresponding to the time surrounding the current sheet crossing (not shown).

Authors=Zhang, H.; Cai, H. T.; Wan, X.; Hu, K.; Xiong, C.; Gao, S. Z.; Yang, L. B.;Title=The Altitudinal Dependences of the Inter-Hemispheric Asymmetry in the Mid-Latitude Ionospheric Post-Midnight Enhancement During Equinox, 2024, doi:10.1029/2023JA032260, ID:26804086.Keywords: space physics data facility, omniwebSample usage ( ACK ) =The authors acknowledge solar ionizing flux ( F 107) and Kp data are available via the Space Physics Data Facility OMNIWeb interface. The authors would like to acknowledge ESA for providing Swarm data, and GFZ for providing CHAMP and GRACE data. The authors would like to acknowledge ESA for providing Swarm data, and GFZ for providing CHAMP and GRACE data. Sample usage ( BODY ) =The Kp and F 107 indices can be obtained in OMNIweb ( https://omniweb.gsfc.nasa.gov/form/dx1.html ). The SAMI2 modeled values are generated using sami2py 0.2.5 (Klenzing et al., 2021, 2022).

Authors=Hodnett, R. M.; Yeoman, T. K.; Beggan, C. D.; Wright, D. M.;Title=Modeling and Observations of the Effects of the Alfven Velocity Profile on the Ionospheric Alfven Resonator, 2024, doi:10.1029/2023JA032308, ID:26804090.Keywords: iri, international reference ionosphereSample usage ( BODY ) =We used the International Reference Ionosphere (IRI) (Bilitza et al., 2017) to estimate the plasma mass density and the International Geomagnetic Reference Field (IGRF) (Alken et al., 2021) to trace the magnetic field lines in order to obtain Alfven velocity profiles. Sample usage ( BODY ) =To model D f , the Alfven velocity was required.

Authors=Liu, Jing; Zhang, Donghe; Li, Quanhan; Tian, Yaoyu; Coster, Anthea; Hao, Yongqiang; Xiao, Zuo;Title=Controlling Factors of the Seasonal Variation of the Latitudinal Location of the Equatorial Ionization Anomaly Crest, 2024, doi:10.1029/2023JA031807, ID:27118500.Keywords: omni, omniwebSample usage ( BODY ) =Kp and Dst indices were from the OMNI data set ( https://omniweb.gsfc.nasa.gov/form/dx1.html ).

Authors=Liu, Yangkun; Xu, Jiyao; Smith, A. K.; Liu, Xiao;Title=Seasonal and Interannual Variations of Global Tides in the Mesosphere and Lower Thermosphere Neutral Winds: II. Semidiurnal and Terdiurnal Tides, 2024, doi:10.1029/2023JA031846, ID:27118502.Keywords: omni, omni-2Sample usage ( BODY ) =The F 10.7 solar radio flux are from the OMNI 2 database ( https://spdf.gsfc.nasa.gov/pub/data/**omni**/low_res_omni/ ).

Authors=Anderson, Phillip C.; Bukowski, Aaron L.;Title=Magnetic Local Time and Interplanetary Magnetic Field By Variation of Cusp Location Dependence on Dipole Tilt, 2024, doi:10.1029/2023JA031886, ID:27118504.Keywords: spdf, space physics data facility, omni, omniwebSample usage ( BODY ) =Data Availability Statement The DMSP particle data are freely available from the NASA Goddard Space Flight Center Space Physics Data Facility at https://spdf.gsfc.nasa.gov/pub/data/dmsp/. The IMF data are freely available from the NASA Goddard Space Flight Center Physics Data Facility OMNIWeb interface at https://omniweb.gsfc.nasa.gov. Sample usage ( BODY ) =We identified the IMF and solar wind parameters associated with each boundary using high resolution data from NASA’s OMNI website (Papitashvili King, 2020) and were able to acquire IMF data for over 40,000 of our remaining boundaries (29,150 in the northern hemisphere and 11,617 in the southern hemisphere).

Authors=Liu, Yangkun; Xu, Jiyao; Smith, A. K.; Liu, Xiao;Title=Seasonal and Interannual Variations of Global Tides in the Mesosphere and Lower Thermosphere Neutral Winds: I. Diurnal Tides, 2024, doi:10.1029/2023JA031887, ID:27118505.Keywords: omni, omni-2Sample usage ( BODY ) =The F 10.7 solar radio flux are from the OMNI 2 database ( https://spdf.gsfc.nasa.gov/pub/data/**omni**/low_res_omni/ ).

Authors=Liu, Terry Z.; Angelopoulos, Vassilis; Vu, Andrew; Zhang, Hui; Otto, Antonius; Zhang, Kun;Title=THEMIS Observations of Magnetosheath-Origin Foreshock Ions, 2024, doi:10.1029/2023JA031969, ID:27118506.Keywords: cdaweb, omniSample usage ( BODY ) =Data Availability Statement THEMIS data set are available at NASA’s Coordinated Data Analysis Web (CDAWeb, http://cdaweb.gsfc.nasa.gov/ ). The SPEDAS software (see Angelopoulos et al. ( 2019)) is available at http://themis.ssl.berkeley.edu. Sample usage ( BODY ) =We analyze plasma data from electrostatic analyzer (ESA) (McFadden et al., 2008) and DC magnetic field data from fluxgate magnetometer (Auster et al., 2008). OMNI data is used for the pristine solar wind data. We calculate foreshock ion moments by removing solar wind ions from ion distribution functions by setting up a velocity radius around the solar wind (see detailed method in Liu et al. ( 2017)).

Authors=Mooney, M. K.; Milan, S. E.; Bower, G. E.;Title=Plasma Observations in the Distant Magnetotail During Intervals of Northward IMF, 2024, doi:10.1029/2023JA031999, ID:27118507.Keywords: cdaweb, space physics data facility, omni, omniwebSample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s CDAWeb service (at http://cdaweb.gsfc.nasa.gov ) and OMNI data (at https://omniweb.gsfc.nasa.gov/html/ow_data.html ). Sample usage ( BODY ) =We also acknowledge the low resolution (5-min) OMNI data used in this study (King Papitashvili, 2005) provided by the NASA Goddard Space Flight Center, Space Physics Data Facility and publicly available at https://omniweb.gsfc.nasa.gov/html/ow_data.html. We are grateful for the insightful comments from V. Sample usage ( BODY ) =In this study, we focus on observations from the ARTEMIS P2 spacecraft although observations from ARTEMIS P1 are also included for completeness. We use data from the OMNI database (King Papitashvili, 2005) to monitor the upstream solar wind conditions throughout the period.

Authors=Zhang, Y.; Gallardo-Lacourt, B.; Paxton, L. J.; Erickson, P. J.; Hairston, M.; Coley, W. R.;Title=STEVE Events With FUV Emissions, 2024, doi:10.1029/2023JA032017, ID:27118508.Keywords: cdaweb, spdf, omniSample usage ( BODY ) =OMNI data and F17 DMSP ion density data were from https://cdaweb.gsfc.nasa.gov/ and select OMNI and DMSP (Candey et al., 2020) THEMIS ASI data can be obtained from https://data.phys.ucalgary.ca/sort_by_project/THEMIS/asi/stream2/2008/03/27/pina_themis18/ (Donovan et al., 2006).Sample usage ( BODY ) =It is interesting to note that the Vx flow (data not shown) was duskward (in the same direction as the spacecraft velocity vector) before, after, and during the STEVE event. 10 Figure F17 DMSP SSIES ion densities observed by four different sensors (PRA, Scintillation Meter, PRA with 0 V, and IDM) during the STEVE event between 03:33:47 and 03:34:12, 27 March 2008. These data are from NASA SPDF website. On the other hand, the ion density data from Retarding Potential Analyzer (RPA) are reliable on either side of the 14 s STEVE event (03:33:48 to 03:34:01, inclusive, green vertical dashed lines) as O + accounts for 70%-100% of the plasma. Sample usage ( BODY ) =This further limits statistics on observations of FUV STEVE events. 3 Table STEVE Events From Ground Visible Imagers Year 2008 2008 2008 2008 2008 2008 2008 2008 2010 Month 02 03 03 03 03 04 05 07 03 Day 11 26 27 28 28 12 04 12 11 UT 09:30 07:20 03:00 02:14 07:22 08:20 08:14 03:40 06:00 Year 2010 2010 2010 2010 2011 2011 2011 2012 2013 Month 04 04 08 09 04 04 06 02 09 Day 04 05 03 17 02 20 23 20 13 UT 07:20 05:30 05:40 08:22 06:47 08:38 07:15 08:40 08:30 Year 2014 2015 2015 2016 2016 2016 2016 2017 2017 Month 08 09 09 02 04 07 07 08 08 Day 21 07 11 08 17 25 29 22 24 UT 09:20 05:35 05:20 06:30 05:10 06:00 05:20 03:08 06:11 Year 2017 2017 2017 2018 2018 2018 2018 Month 09 09 08 03 04 05 07 Day 18 27 20 25 10 07 17 UT 06:35 06:41 02:12 07:46 05:10 04:25 06:30 Solar Wind and IMF Condition Associated With the FUV STEVE Events Figure 11 shows OMNI solar wind, IMF and geomagnetic SymH and AE index on March 26 and 27, 2008.

Authors=Xirogiannopoulou, N.; Goncharov, O.; A afrankova, J.; Nemecek, Z.;Title=Characteristics of Foreshock Subsolar Compressive Structures, 2024, doi:10.1029/2023JA032033, ID:27118510.Keywords: space physics data facility, omni, omniwebSample usage ( ACK ) =We also acknowledge NASA’s National Space Science Data Center and Space Physics Data Facility.Sample usage ( BODY ) =OMNI data is available from NASA Goddard Flight Center’s Space Physics Data Facility https://omniweb.gsfc.nasa.gov/ (King Papitashvili, 2005). Sample usage ( BODY ) =The upstream solar wind parameters were obtained from the high resolution 1-min OMNI data propagated to the bow shock nose ( https://omniweb.gsfc.nasa.gov/ow_min.html ). Sample usage ( ABSTRACT ) =Using measurements of the Magnetospheric Multiscale Spacecraft (MMS) and OMNI solar wind database between the 2015 and 2018 years, we have found that there is a category of events exhibiting both magnetic field and density enhancements simultaneously and we introduce the term “mixed structures” for them. To decrease the influence of the uncertainty of the solar wind propagation from the L1 point to the BS, all upstream solar wind parameters were averaged over 2 min before and after the registration of the structures.

Authors=Bag, Tikemani; Ogawa, Y.;Title=Response Time of Joule Heating Rate and Nitric Oxide Cooling Emission During Geomagnetic Storms: Correlated Ground-Based and Satellite Observations, 2024, doi:10.1029/2023JA032072, ID:27118512.Keywords: omniwebSample usage (ACK) =Acknowledgments The authors thank the TIMED/SABER science team ( https://saber.gats-inc.com/ ), OMNIweb ( https://omniweb.gsfc.nasa.gov/ ), EISCAT (https://eiscat.se/) and CCMC (https://ccmc.gsfc.nasa.gov/) for providing the data used in this study. Sample usage ( BODY ) =The modified 1-min resolution solar wind and interplanetary magnetic field data are obtained from the OMNIweb (https://omniweb.gsfc.nasa.gov/form/omni_min_def.html). The data with 1-min resolution is definitive Wind/SWE plasma shifted to Bow shock nose which involves the combination of the data from Bow Shock shifted ACE, wind, IMP8 and Geotail spacecrafts.

Authors=Tuminello, Richard M.; Stephan, Andrew W.; England, Scott L.;Title=Retrieval of Thermospheric O and N2 Densities From ICON EUV, 2024, doi:10.1029/2023JA032100, ID:27118516.Keywords: cdaweb, space physics data facilitySample usage ( BODY ) =These data are available for download from the ICON website hosted by the Berkeley Space Sciences Laboratory ( https://icon.ssl.berkeley.edu/Data ) and from the NASA Space Physics Data Facility https://cdaweb.gsfc.nasa.gov/pub/data/icon/. This study uses version 01 of the Swarm-C Accelerometer Derived Density data (March et al., 2021), available for download from ESA ( https://swarm-diss.eo.esa.int/ ).

Authors=Guo, Wenlong; Tang, Binbin; Zhang, Qinghe; Li, Wenya; Yang, Zhongwei; Sun, Tianran; Ma, Jiuqi; Zhang, Xiaoxin; Liu, Ziqian; Guo, Xiaocheng; Wang, Chi;Title=The Magnetopause Deformation Indicated by Fast Cold Ion Motion, 2024, doi:10.1029/2023JA032121, ID:27118517.Keywords: cdaweb, omniSample usage ( BODY ) =Data Availability Statement MMS data are available at the MMS Science Data Center ( https://lasp.colorado.edu/mms/sdc/public/about/browse-wrapper/ ), and the solar wind data are accessible at the CDAweb ( https://cdaweb.gsfc.nasa.gov/pub/data/ ). The IRFU-Matlab package ( https://github.com/irfu/irfu-matlab ) is used for data analysis. Sample usage ( BODY ) =Finally, the solar wind parameters from OMNI should be stable at least for 15 min surrounding the magnetopause crossing, meaning the standard deviation of the interplanetary magnetic field B Z , plasma number density and the x component of solar wind velocity does not exceed 1.5 nT, 0.5 cm -3 and 15 km s -1 respectively, so that we can exclude the impact of the solar wind structures (such as magnetic discontinuities) to the magnetopause. If there are data gaps in the OMNI data set, we use time-shifted ACE data instead. Figure 1 shows locations of 30 selected MMS magnetopause crossings from 2015 to 2021.

Authors=Teng, S.; Zhang, Q.; Zhou, Su; Wang, Z.; Han, Desheng;Title=Conjugate Observations of Magnetospheric and Ionospheric Phenomena During a Substorm Event, 2024, doi:10.1029/2023JA032134, ID:27118518.Keywords: cdaweb, spdf, omniSample usage ( BODY ) =Data of interplanetary parameters are available on the CDAWEB from https://spdf.gsfc.nasa.gov/pub/data/omni/. Van Allen Probes data is available at https://spdf.gsfc.nasa.gov/pub/data/rbsp/. Van Allen Probes data is available at https://spdf.gsfc.nasa.gov/pub/data/rbsp/. Sample usage ( BODY ) =The Electric Field and Waves (EFW) instruments measure the electric field at a sampling rate of 32 Hz (Wygant et al., 2014). Omni-directional electron/proton energy fluxes were measured using Helium, Oxygen, Proton and Electron (HOPE) (Funsten et al., 2013) mass spectrometer and the Radiation Belt Storm Probes Ion Composition Experiment (RBSPICE) instrument (Mitchell et al., 2013).

Authors=Gu, Wenyao; Hartley, David; Liu, Xu; Chen, Lunjin; Bortnik, Jacob; Horne, Richard B.;Title=Propagation of Very Oblique Chorus Waves Near a Plasmaspheric Plume Boundary, 2024, doi:10.1029/2023JA032151, ID:27118519.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement Data from Van Allen Probes can be assessed from https://cdaweb.gsfc.nasa.gov/. Ray-tracing results data can be downloaded from https://doi.org/10.5281/zenodo.8381779.

Authors=Yang, Yuyan; Liu, Libo; Li, Wenbo; Chen, Yiding; Le, Huijun; Zhang, Ruilong; Zhao, Xiukuan;Title=Localized Plasma Density Peak at Middle Latitudes During the April 2023 Geomagnetic Storm, 2024, doi:10.1029/2023JA032165, ID:27118523.Keywords: omni, omniwebSample usage ( BODY ) =The 1-min averaged V, P, By, Bz, Ey, and SYM-H data are downloaded from the OMNI database available at https://omniweb.gsfc.nasa.gov/. AE indices data are archived at the World Data Center for Geomagnetism, Kyoto ( http://wdc.kugi.kyoto-u.ac.jp/index.html ).

Authors=Wang, Hui; Sun, Yu; Luhr, Hermann;Title=Interplanetary Magnetic Field By Effects on the Strength and Latitude of Field-Aligned Currents in Different Magnetic Local Time Sectors, 2024, doi:10.1029/2023JA032188, ID:27118525.Keywords: space physics data facility, omniwebSample usage ( BODY ) =The solar wind and interplanetary magnetic field and magnetic activity index data are from NASA/GSFC’S Space Physics Data Facility’s OMNIWeb ( https://omniweb.gsfc.nasa.gov ).

Authors=Decotte, Margot; Laundal, Karl M.; Hatch, Spencer M.; Reistad, Jone P.;Title=Occurrence Probability of Magnetic Field Disturbances Measured With Swarm: Mapping the Dynamic Magnetosphere-Ionosphere Coupling, 2024, doi:10.1029/2023JA032191, ID:27118529.Keywords: spdf, omniSample usage ( ACK ) =We acknowledge the use of NASA/GSFC SPDF service to obtain these data. We also acknowledge the substorm timing list identified by the Ohtani and Gjerloev technique (Ohtani Gjerloev, 2020), the SMU and SML indices (Newell Gjerloev, 2011); and the SuperMAG collaboration (Gjerloev, 2012).Sample usage ( BODY ) =The OMNI data, including the solar wind data and geomagnetic activity indices, are available on the NASA/GSFC SPDF interface (Papitashvili, 2005).Sample usage ( ACK ) =Papitashvili for the multi-sources OMNI data. Sample usage ( BODY ) =As we aim to investigate how the disturbed magnetic field behaves under various geomagnetic conditions, we combine our Swarm data set with the solar wind magnetic field and plasma parameters from the OMNI database. We point out that these data represent near-Earth estimates of solar wind properties as the original upstream observations have been time-shifted to the Earth’s bow shock nose (King Papitashvili, 2005).

Authors=Li, Xing-Yu; Liu, Zhi-Yang; Zong, Qiu-Gang; Zhou, Xu-Zhi; Liu, Jian-Jun; Hu, Ze-Jun; Zhao, Xing-Xin; Hao, Yi-Xin; Liu, Ying; Yang, Fan; Pollock, Craig J.; Russell, Christopher T.; Lindqvist, Per-Arne;Title=Ion Acceleration and Corresponding Bounce Echoes Induced by Electric Field Impulses: MMS Observations, 2024, doi:10.1029/2023JA032273, ID:27118535.Keywords: cdaweb, space physics data facility, omniSample usage ( BODY ) =We thank Space Physics Data Facility at NASA Goddard Space Flight Center ( https://cdaweb.gsfc.nasa.gov/index.html/ ) for providing Wind and ARTEMIS data, including magnetic field data from the Magnetic Field Investigation (MFI, Wind), ion moments data from the 3-D Plasma and Energetic Particle Investigation (3DP, Wind), magnetic field data from the Fluxgate Magnetometer (FGM, ARTEMIS) and ion data from the Electrostatic Analyzer (ESA, ARTEMIS). Sample usage ( BODY ) =(a) The energy-time spectrogram of omni-directional ion energy fluxes, obtained by FPI (b)-(d) Components of the ion bulk velocity in geocentric solar ecliptic (GSE) coordinates, measured by FPI (e)-(f) The magnetic field strength (e) and components in GSE coordinates (f), obtained by FGM.

Authors=Gasque, L. Claire; Harding, Brian J.; Immel, Thomas J.; Wu, Yen-Jung; Triplett, Colin C.; Vadas, Sharon L.; Becker, Erich; Maute, Astrid; Title=Evening Solar Terminator Waves in Earth’s Thermosphere: Neutral Wind Signatures Observed by ICON-MIGHTI, 2024, doi:10.1029/2023JA032274, ID:27118536.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement This analysis used ICON/MIGHTI neutral wind data, Level 2.2, Version 5, which is available from https://icon.ssl.berkeley.edu/Data and https://cdaweb.gsfc.nasa.gov/pub/data/icon/ (Harding et al., 2023a, 2023b). The WACCM-X simulations used in this work are available from https://doi.org/10.5065/rjgt-g951 (Maute HAO WACCM team, 2022). The TIEGCM-ICON simulations Level 4 V01 are available at https://cdaweb.gsfc.nasa.gov/pub/data/icon/l4/ (Maute ICON Team, 2022). The HIAMCM simulation is available at https://www.cora.nwra.com/vadas/Vadas-etal-JGR-2023-TongaICON-files/ (Becker Vadas, 2022).

Authors=Lee, Sang-Yun; Tu, Weichao; Cunningham, Gregory S.; Cowee, Misa M.; Wang, Dedong; Shprits, Yuri Y.; Henderson, Michael G.; Reeves, Geoffrey D.;Title=Simulating Long-Term Dynamics of Radiation Belt Electrons Using DREAM3D Model, 2024, doi:10.1029/2023JA032286, ID:27118537.Keywords: cdaweb, omniSample usage ( BODY ) =Geomagnetic activity indices were obtained from the NASA OMNI Web ( https://cdaweb.gsfc.nasa.gov/ ). The PSD data and simulation results presented in this study are publicly available at Zenodo (Lee et al., 2024). The PSD data and simulation results presented in this study are publicly available at Zenodo (Lee et al., 2024).

Authors=Tong, Xin; Liu, Wenlong; Zhang, Dianjun; Sarris, Theodore; Li, Xinlin; Zhang, Zhao; Yan, Li;Title=Statistical Study on the Azimuthal Mode Number of Pc5 ULF Wave in the Inner Magnetosphere, 2024, doi:10.1029/2023JA032306, ID:27118540.Keywords: omni, omniwebSample usage ( BODY ) =Methodology This work uses magnetic field measurements provided by Geostationary Operational Environmental Satellites (GOES) and solar wind parameters from OMNI. The GOES satellites orbit the Earth in the geosynchronous orbit, which allows these satellites to maintain a constant distance from the Earth (geocentric distance = 6.6 R E ). Sample usage ( ACK ) =We would thank NASA/Goddard Space Flight Center for public solar wind data and geomagnetic indices at OmniWeb. We acknowledge Sebastian Krieger and other contributors for available wavelet and cross-wavelet software. Sample usage ( BODY ) =Solar wind parameter data and geomagnetic indices are available at OmniWeb ( https://omniweb.gsfc.nasa.gov/ ). Cross-wavelet software is publicly available at the link https://github.com/regeirk/pycwt.

Authors=Wang, Xin; Cai, Lei; Aikio, Anita; Vanhamaki, Heikki; Virtanen, Ilkka; Zhang, Yongliang; Luo, Bingxian; Liu, Siqing;Title=Ionospheric Conductances Due To Electron and Ion Precipitations: A Comparison Between EISCAT and DMSP Estimates, 2024, doi:10.1029/2023JA032354, ID:27118541.Keywords: omniwebSample usage ( BODY ) =The solar radiation proxy F10.7 is obtained from https://omniweb.gsfc.nasa.gov/form/dx1.html. The open source Python package GeospaceLAB is used to search for EISCAT-DMSP conjugate events and to visualize the data (Cai et al., 2022).

Authors=Pump, K.; Heyner, D.; Schmid, D.; Exner, W.; Plaschke, Ferdinand;Title=Revised Magnetospheric Model Reveals Signatures of Field-Aligned Current Systems at Mercury, 2024, doi:10.1029/2023JA031529, ID:27466614.Keywords: omniSample usage ( BODY ) =The simulation output is based on the OMNI solar wind 1-hr data (King Papitashvili, 2005) of solar wind variations observed near the Earth and propagated back to Mercury’s position, using a 1-dimensional magnetohydrodynamic (MHD) model.

Authors=Michael, C. M.; Yeoman, T. K.; Wright, D. M.; Chelpanov, M. A.; Mager, P. N.;Title=Evolving Phase Propagation in an Intermediate-m ULF Wave Driven by Substorm-Injected Particles, 2024, doi:10.1029/2023JA031654, ID:27466616.Keywords: cdawebSample usage ( BODY ) =Data from Themis A (see https://cdaweb.gsfc.nasa.gov/ ) in the dusk sector shows evidence of dispersed ion signatures between ~10 - 20 keV close to 00:00 UT.

Authors=Kumar, S.; Pulkkinen, T. I.; Gjerloev, J.;Title=Magnetotail Variability During Magnetospheric Substorms, 2024, doi:10.1029/2023JA031722, ID:27466618.Keywords: spdf, space physics data facility, omni, omniwebSample usage ( BODY ) =Data Availability Statement All data used in this study are openly available from the NASA Space Physics Data Facility (SPDF, https://spdf.gsfc.nasa.gov/ ) and the SuperMAG website ( https://supermag.jhuapl.edu/ ). Sample usage ( BODY ) =The magnetometer data has been augmented by the OMNI ( https://omniweb.gsfc.nasa.gov/ ) data set of solar wind and interplanetary magnetic field measurements time-shifted to the Earth’s bow shock (King, 2005) for context.

Authors=Cahyadi, Mokhamad Nur; Muslim, Buldan; Muafiry, Ihsan Naufal; Gusman, Aditya Riadi; Handoko, Eko Yuli; Anjasmara, Ira Mutiara; Putra, Meilfan Eka; Wulansari, Mega; Lestari, Dwi Sri; Jin, Shuanggen; Sri Sumantyo, Josaphat Tetuko;Title=3D Traveling Ionospheric Disturbances During the 2022 Hunga Tonga-Hunga Ha’apai Eruption Using GNSS TEC, 2024, doi:10.1029/2023JA031806, ID:27466623. Keywords: iriSample usage ( BODY ) =The vertical profile of electron density was also estimated on 15 January 2022, and the time TIDs occurred in each location using the IRI model ( https://irimodel.org/ ). The results indicated that the highest electron density was at an altitude of ~280-350 km, as presented in Figure 12, and this is in line with the 3D tomography modeling applied at the height of the third ionospheric layer with an altitude of ~300 km (Chapman, 1931).

Authors=Calabia, Andres.; Imtiaz, Nadia; Altadill, David; Yasyukevich, Yury; Segarra, Antoni; Prol, Fabricio S.; Adhikari, Binod; del Peral, Luis; Rodriguez Frias, Maria Dolores; Molina, Inigo;Title=Uncovering the Drivers of Responsive Ionospheric Dynamics to Severe Space Weather Conditions: A Coordinated Multi-Instrumental Approach, 2024, doi:10.1029/2023JA031862, ID:27466627.Keywords: omni, omniweb, iri, international reference ionosphere. Sample usage ( BODY ) =The solar wind parameters and PCN index are obtained from the NASA OMNI website ( http://omniweb.gsfc.nasa.gov/ ), the Am index (Mayaud et al., 2023) is obtained from the EOST (Ecole and Observatoire des Sciences de la Terre) ( https://eost.unistra.fr/en/eost/eost ), and the AE (Davis Sugiura, 1966) and SYM-H (Zhao et al., 2021) indices are obtained from the World Data Center Kyoto ( https://wdc.kugi.kyoto-u.ac.jp/ ). Sample usage ( BODY ) =For our experiment, we set the model to a constant quiet geomagnetic contribution (Am = 6) and the results are compared with the IRI-2020. It’s important to note that some attenuation may occur due to missing contributions from the full plasmasphere (Jin et al., 2021). Sample usage ( BODY ) =We use predictive ionospheric models to investigate abrupt ionospheric anomalies during geomagnetic storms, the empirical model developed at Calabia and Jin ( 2019, 2020), which is based on a lower-dimensional reduction of vertical Total Electron Content (vTEC) data from 2003 to 2018, and the International Reference Ionosphere (IRI-2020) model (Bilitza et al., 2022), which specifies monthly averages of electron density, ion composition, electron temperature, and ion temperature in the altitude range of 50-2,000 km.

Authors=Zhang, Shuai; Rae, I. Jonathan; Liu, Kaijun; Watt, Clare E. J.; Shi, Quanqi; Tian, Anmin; Degeling, Alexander W.; Guo, Ruilong; Wang, Mengmeng; Shen, Xiao-Chen; Yao, Fei; Li, Jing chun;Title=Effects of Plasma Density on the Spatial and Temporal Scale Sizes of Plasmaspheric Hiss, 2024, doi:10.1029/2023JA031955, ID:27466632.Keywords: spdfSample usage ( BODY ) =Data Availability Statement We acknowledge the Van Allen Probes instrument team, and the data are open availability at: https://spdf.gsfc.nasa.gov/ .

Authors=Wu, Chen; Ridley, Aaron J.;Title=Auroral Characteristics Related to AU&AL Indices, 2024, doi:10.1029/2023JA032002, ID:27466637.Keywords: spdf, space physics data facility, omniwebSample usage ( BODY ) =The AE, AU, and AL indices, the interplanetary magnetic field data, and the solar wind data were provided by the NASA/GSFC’s Space Physics Data Facility’s OMNIWeb service ( https://spdf.gsfc.nasa.gov/ ). The EDR-AUR SSUSI data were provided by the website of Special Sensor Ultraviolet Spectrographic mager ( https://ssusi.jhuapl.edu/ ).

Authors=Laitinen, J.; Holappa, L.; Vanhamaki, H.;Title=A Combined Effect of the Earth’s Magnetic Dipole Tilt and IMF By in Controlling Auroral Electron Precipitation, 2024, doi:10.1029/2023JA032040, ID:27466639.Keywords: omni2, omni-2, omniwebSample usage ( BODY ) =The solar wind data was downloaded from the OMNI2 database ( http://omniweb.gsfc.nasa.gov/ ).

Authors=Grimmich, Niklas; Prencipe, Fabio; Turner, Drew L.; Liu, Terry Z.; Plaschke, Ferdinand; Archer, Martin O.; Nakamura, Rumi; Sibeck, David G.; Mieth, Johannes Z. D.; Auster, Hans-Ulrich; Constantinescu, O. Dragos; Fischer, David; Magnes, Werner;Title=Multi Satellite Observation of a Foreshock Bubble Causing an Extreme Magnetopause Expansion, 2024, doi:10.1029/2023JA032052, ID:27466644.Keywords: omni, omni-2Sample usage ( ACK ) =Papitashvili of the National Space Science Data Center (NSSDC) in the NASA/GSFC for the use of the OMNI 2 database, and also N. Ness and D. McComas for the use of the ACE data. Sample usage ( BODY ) =Data and Methods For our analysis, we utilize a wide range of different spacecraft data: Magnetometer data with a 1 s cadence from the Advanced Composition Explorer (ACE, Stone et al., 1998; Smith et al., 1998) located far upstream at L1 around [217.57, -9.17, 17.16] R E and time-shifted high resolution OMNI data with a cadence of 1 min (King Papitashvili, 2005) are used to monitor upstream conditions of the solar wind.

Authors=Li, Hui; Liu, Xiaodong; Wang, Chi;Title=How Solar Wind Controls the Recovery Phase Morphology of Intense Magnetic Storms, 2024, doi:10.1029/2023JA032057, ID:27466646.Keywords: cdaweb, omniSample usage ( BODY ) =The OMNI data and the Wind data from https://cdaweb.gsfc.nasa.gov/pub/data/wind/; Dst data from https://wdc.kugi.kyoto-u.ac.jp/ .Sample usage ( BODY ) =Data Availability Statement Publicly available data sets were analyzed in this study.

Authors=Lee, Jae-Hee; Kim, Khan-Hyuk; Baek, Seul-Min; Jin, Ho; Saito, Yoshifumi; Nishino, Masaki N.; Yokota, Shoichiro;Title=The Relationship Between the Energization of Moon-Originating Ions and Terrain Type on the Lunar Surface, 2024, doi:10.1029/2023JA032076, ID:27466651.Keywords: omniwebSample usage ( BODY ) =Solar X-ray fluxes data from GOES are provided by OMNIWeb ( http://omniweb.gsfc.nasa.gov ). The data analysis was conducted using version 5.0 of the Space Physics Environment Data Analysis System (SPEDAS), which is available on the THEMIS website ( http://themis.ssl.berkeley.edu/software.shtml ).

Authors=Hu, Lianhuan; Li, Guozhu; Ning, Baiqi; Sun, Wenjie; Xie, Haiyong; Zhao, Xiukuan; Li, Yi; Dai, Guofeng; Xiao, Qi; Yan, Yong;Title=Development of Low Latitude Long Range Ionospheric Radar f or Observing Plasma Bubble Irregularities and Preliminary Results, 2024, doi:10.1029/2023JA032099, ID:27466654.Keywords: iri, international reference ionosphereSample usage ( BODY ) =The background ionospheric condition was derived from the International Reference Ionosphere model (IRI-2012) (Bilitza et al., 2014). The sunspot number (SSN) used in the IRI model are 70 and 150 for low and high solar activities, respectively.

Authors=Kamaletdinov, S. R.; Artemyev, A. V.; Runov, A.; Angelopoulos, V.;Title=Thin Current Sheets in the Magnetotail at Lunar Distances: Statistics of ARTEMIS Observations, 2024, doi:10.1029/2023JA03213010.48550/arXiv.2309.16194, ID:27466657.Keywords: omniSample usage ( BODY ) =As a result, we can statistically assess the impact of solar wind dynamics on the magnetotail at lunar distances. We employ the OMNI data (King Papitashvili, 2005), at 1 min resolution, providing us with the Interplanetary Magnetic Field IMF B = IMF ( B x , B y , B z ).

Authors=Nykiel, Grzegorz; Ferreira, Arthur; Gunzkofer, Florian; Iochem, Pelin; Tasnim, Samira; Sato, Hiroatsu;Title=Large-Scale Traveling Ionospheric Disturbances Over the European Sector During the Geomagnetic Storm on March 23-24, 2023: Energy Deposition in the Source Regions and the Propagation Characteristics, 2024, doi:10.1029/2023JA032145, ID:27466659.Keywords: cdaweb, space physics data facility, omni, omniwebSample usage ( BODY ) =The WIND spacecraft data from 21 to 25 March 2023, were downloaded from the Automated Multi Dataset Analysis system (AMDA) and Coordinated Data Analysis Web (CDAWeb) of NASA. The information related to the Coronal Mass Ejection (CME) events of 20 March 2023, was collected from the LASCO (Large Angle and Spectrometric Coronagraph Experiment) instrument on board the SOHO (Solar and Heliospheric Observatory) mission. Sample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s OMNIWeb. We are grateful to the AMDA science analysis system provided by the Centre de Donnees de la Physique des Plasmas (CDPP) supported by CNRS, CNES, Observatoire de Paris and Universite Paul Sabatier, Toulouse. Sample usage ( BODY ) =Solar wind input data is taken from OMNI. The input parameter for radio flux 10.7 cm is given as 157 for the model, the average daily value between start and end date of the run. Sample usage ( BODY ) =It displays the magnetic hodogram of the GSE components B y and B z . A line (red) using hourly OMNIWeb data is overplotted. The start and end of the period are marked using black and magenta squares, respectively.

Authors=Hao, Honglian; Zhao, Biqiang; Jin, Yuyan; Yue, Xinan; Ding, Feng; Li, Guozhu; Sun, Wenjie; Ren, Zhipeng; Li, Zishen;Title=Latitude Variation of the Post-Sunset Plasma Density Enhancement During the Minor Geomagnetic Storm on 27 May 2021, 2024, doi:10.1029/2023JA032156, ID:27466661.Keywords: omniSample usage ( BODY ) =The solar wind data with a time resolution of 1 min is obtained from the OMNI database. The Kp index with a temporal resolution of 3 hr and the F10.7 index with a resolution of 1 day are provided by the German Geosciences Center.

Authors=Li, Zhi-Gu; Tu, Weichao; Selesnick, Richard; Huang, Jinbei;Title=Modeling the Contribution of Precipitation Loss to a Radiation Belt Electron Dropout Observed by Van Allen Probes, 2024, doi:10.1029/2023JA032171, ID:27466665.Keywords: omniwebSample usage ( BODY ) =Van Allen Probes MagEIS and REPT data are available online ( https://spdf.gsfc.nasa.gov/pub/data/rbsp/rbspa/l3/ect/ ). NASA’s OMNIWeb data is available at ( https://omniweb.gsfc.nasa.gov/ ). The model results of the electron distribution functions per each simulation interval, as well as the MPE data set files used specifically in this study are also available online publicly ( https://doi.org/10.5281/zenodo.10694739 ).

Authors=Liu, Yunbo; Ren, Zhipeng; Wei, Yong; Zhou, Xu;Title=A Simulation Study of the Modulation of the Geomagnetic Field Configuration on the Seasonal Variation of Ionospheric Sq Currents, 2024, doi:10.1029/2023JA032180, ID:27466667.Keywords: iriSample usage ( BODY ) =The initial conditions of the temperature and density of electrons and ions for this model are mainly derived from the MSIS00, IRI empirical models. The HWM93 empirical model is incorporated into the model solely to serve as the initial condition for F-layer neutral wind (>150 km), while the initial condition for E-layer neutral wind is set to zero.

Authors=Shaver, S. R.; Solt, L.; Andersson, L.; Halekas, J.; Jian, L.; da Silva, D. E.; Jolitz, R.; Malaspina, D.; Fowler, C. M.; Ramstad, R.; Lillis, R.; Xu, S.; Azari, A. R.; Mazelle, C.; Rahmati, A.; Lee, C. O.; Hesse, T.; Hamil, O.; Pilinski, M.; Brain, D.; Garnier, P.; Cravens, T. E.; McFadden, J. P.; Hanley, K. G.; Mitchell, D. L.; Espley, J. R.; Gruesbeck, J. R.; Larson, D.; Curry, S.;Title=The Martian Ionospheric Response to the Co-Rotating Interaction Region That Caused the Disappearing Solar Wind Event at Mars, 2024, doi:10.1029/2023JA032181, ID:27466669.Keywords: omniwebSample usage ( BODY ) =The MAVEN data used in this study are available through the Planetary Data System https://pds-ppi.igpp.ucla.edu/mission/MAVEN, Wind data is available through NASA’s OMNIWeb site https://omniweb.gsfc.nasa.gov/ , and the ADAPT-WSA ensemble set used for solar wind footpoints can be found at https://wsa-dashboard.helioanalytics.io/footpoint .

Authors=Pignalberi, A.; Giannattasio, F.; Truhlik, V.; Coco, I.; Pezzopane, M.; Alberti, T.;Title=Investigating the Main Features of the Correlation Between Electron Density and Temperature in the Topside Ionosphere Through Swarm Satellites Data, 2024, doi:10.1029/2023JA032201, ID:27466671.Keywords: omniweb, iri, international reference ionosphereSample usage ( BODY ) =K p geomagnetic activity index is available from OMNIWeb Data Explorer website ( https://omniweb.gsfc.nasa.gov/form/dx1.html ). Sample usage ( BODY ) =Indeed, in the 60s and 70s the knowledge of the horizontal distribution of N e at the F2-layer peak (the absolute maximum of N e in the ionosphere), on a global scale, was already well-established through the works of Jones and Gallet ( 1962, 1965), and the corresponding vertical profile modeled through the first implementations of the International Reference Ionosphere (IRI) model (Bilitza et al. ( 2022) and references therein). This is why early representations of T e in the IRI model relied on its anti-correlation with N e (Bilitza, 1975, 1983).

Authors=Virtanen, Ilkka I.; Tesfaw, Habtamu W.; Aikio, Anita T.; Varney, Roger; Kero, Antti; Thomas, Neethal;Title=F1 Region Ion Composition in Svalbard During the International Polar Year 2007-2008, 2024, doi:10.1029/2023JA032202, ID:27466672.Keywords: iri, international reference ionosphereSample usage ( BODY ) =Underestimation of F 1 region N e by previous versions of IRI in Svalbard has been reported by (Bjoland et al., 2016). One can also see that the IRI z 50 is controlled by the IRI N e variations, which may be expected as the IRI T i is almost constant. Sample usage ( BODY ) =The same chemistry model is used also in the latest versions of the International Reference Ionosphere (Bilitza et al., 2022). In this paper we combine the BAFIM tool (Virtanen et al., 2021) with the IDC (Richards, 2011; Richards et al., 2010) to carry out IS radar data analysis in a way that produces reliable estimates of the fraction of O + ions and ion temperature in the F region. Sample usage ( ABSTRACT ) =The annual medians of the fitted transition altitudes are 14-32 km lower than those predicted by the International Reference Ionosphere.

Authors=He, Qingbao; Liu, Kaijun; Wang, Zhichao; Liu, Qinghui; Guo, Li;Title=Large TEC Variations Between Mars and Earth: Simulation and Observation Comparisons, 2024, doi:10.1029/2023JA032212, ID:27466674.Keywords: spdf, omni, omniwebSample usage ( BODY ) =Data Availability Statement The OMNI data were obtained from the GSFC/SPDF OMNIWeb interface at https://omniweb.gsfc.nasa.gov. The solar wind structure images and solar wind density in WSA-Enlil model were obtained from https://www.ngdc.noaa.gov/enlil/. Sample usage ( BODY ) =The in situ measurements of STEREO-A are obtained from the OMNI website (Papitashvili King, 2020). CME The large TEC changes observed by Tianwen-1 DOR signals on 23 March 2021 and 18 June 2021 have been shown to be caused by two CMEs passing through the DOR signal path on these days (He et al., 2022).

Authors=Wei, Yafei; Gu, Sheng-Yang; Li, Na; Qin, Yusong; Sun, Ruidi; Wang, Dong; Hu, Guoyuan; Le, Huijun; Yuan, Wei;Title=Passive Optical Observation of Mesosphere and Thermosphere Wind Over Three Stations in China, 2024, doi:10.1029/2023JA032214, ID:27466676.Keywords: omniwebSample usage ( BODY ) =Dst index and f10.7 index are downloaded from https://omniweb.gsfc.nasa.gov/form/dx1.html .

Authors=Archana, R. K.; Arora, Kusumita;Title=Variations of Inter-Hemispheric Field-Aligned Currents: Observations From Ground Geomagnetic Measurements, 2024, doi:10.1029/2023JA032254, ID:27466682.Keywords: omniSample usage ( ACK ) =We thank GFZ for Kp index data, OMNI site for Sunspot numbers and F10.7 values.

Authors=Habarulema, John Bosco; Zhang, Yongliang; Matamba, Tshimangadzo; Buresova, Dalia; Lu, Gang; Katamzi-Joseph, Zama; Fagundes, Paulo Roberto; Okoh, Daniel; Seemala, Gopi;Title=Absence of High Frequency Echoes From Ionosondes During the 23-25 April 2023 Geomagnetic Storm; What Happened?, 2024, doi:10.1029/2023JA032277, ID:27466684.Keywords: omni, omniwebSample usage ( BODY ) =To show the storm evolution, we display three solar wind parameters namely; solar wind velocity, the Bz component of the interplanetary magnetic field (IMF Bz) and solar wind dynamic pressure (P sw ) obtained from the OMNI database ( https://spdf.gsfc.nasa.gov/pub/data/**omni**/high_res_omni/ ). Sample usage ( BODY ) =SYM-H data were downloaded from https://omniweb.gsfc.nasa.gov/form/dx1.html. TIMED/GUVI O/N 2 data were downloaded from http://guvitimed.jhuapl.edu/data_fetch_l3_on2_netcdf .

Authors=Zhao, Shufan; Liao, Li; Shen, Xuhui; Lu, Hengxin;Title=Solar Cycle Variation of Radiated Electric Field and Ionospheric Reflection Height Over NWC Transmitter During 2005-2009: DEMETER Spacecraft Observations and Simulations, 2024, doi:10.1029/2023JA032282, ID:27466685.Keywords: iri, international reference ionosphereSample usage ( BODY ) =In this work, the electron density is calculated by the IRI-2016 (International Reference Ionosphere-2016) model (Bilitza et al., 2017), and the electron collision frequency is modeled by the exponential decay law with the height increasing. Sample usage ( ABSTRACT ) =The difference in the simulated electric field based on the electron density profile from the IRI-2016 model between 2005 and 2009 is lower compared with the observation results.

Authors=Byrd, Susanne; Girazian, Zachary; Ruhunusiri, Suranga;Title=Properties of Mars’ Dayside Low-Altitude Induced Magnetic Field and Comparisons With Venus, 2024, doi:10.1029/2023JA032343, ID:27466689.Keywords: cdawebSample usage ( BODY ) =f=yes/id=pds://PPI/PVO-V-OMAG-4-SCCOORDS-24SEC-V2.0 and the Venus upstream solar wind data can be found at https://cdaweb.gsfc.nasa.gov/cgi-bin/eval1.cgi. The Mars Key Parameters data can be found at https://lasp.colorado.edu/maven/sdc/public/data/sci/kp/ and the Mars upstream solar wind data can be found at https://homepage.physics.uiowa.edu/~jhalekas/drivers.html.

Authors=Bai, Shi-Chen; Shi, Quanqi; Shen, Xiao-Chen; Tian, Anmin; Zhang, Hui; Guo, Ruilong; Wang, Mengmeng; Degeling, Alexander W.; Bu, Yude; Zhang, Shuai; Ma, Xiao;Title=Whistler-Mode Waves Inside Short Large-Amplitude Magnetic Field Structures: Characteristics and Generation Mechanisms, 2024, doi:10.1029/2023JA032392, ID:27466693.Keywords: omniSample usage ( BODY ) =(a) Magnetic fields in the Geocentric Solar Magnetospheric (GSM) coordinate system; (b) electron number density; (c) omni-directional ion energy flux (in the units of keV/cm 2 /s/str/keV); (d) power spectral density of magnetic field and the magenta curve denotes the average frequency < f > of the wave; (e) the degree of polarization; (f) the ellipticity; (g) the planarity, the black dashed curves in (d)-(g) denote the 0.1 f ce , 0.5 f ce , and f ce , respectively and the magenta curve denotes the average frequency < f > of the wave; (h) B w 2 ${\boldsymbol{B}}_{\boldsymbol{w}}^{\mathbf{2}}$ when the criteria of whistler-mode waves are satisfied (shown by red dots) or not (black dots).

Authors=Moges, Samson T.; Sherstyukov, Ruslan O.; Kozlovsky, Alexander; Ulich, Thomas; Lester, Mark;Title=Statistics of Traveling Ionospheric Disturbances at High Latitudes Using a Rapid-Run Ionosonde, 2024, doi:10.1029/2023JA031694, ID:27825257.Keywords: iri, international reference ionosphereSample usage ( BODY ) =We discuss each of these in detail in turn. 4 Figure (a) The occurrence rate distribution of MSTID with IRI-2016 provided hmF2 (Top axis) for Sodankyla during December (black solid line) and July (white solid line) are overlaid. Sample usage ( BODY ) =Daytime MSTIDs frequently appear in winter and for that season MSTID occurrence rate agrees with the hmF2 estimates of the International Reference Ionosphere (IRI-2016) model. The MSTIDs occurrence rate is higher (lower) for the MSTIDs detected at lower (higher) heights.

Authors=Cardenas-O’Toole, Alanah M.; Zou, Shasha; Ren, Jiaen; Wang, Zihan; Jayachandran, P. T.;Title=Phase and Amplitude Scintillations Associated With Polar Cap Patches: Statistical and Event Analyses, 2024, doi:10.1029/2023JA031765, ID:27825259.Keywords: omniwebSample usage ( BODY ) =The solar wind data were provided by the NASA OMNIWeb service ( http://omniweb.gsfc.nasa.gov ). The ionospheric FAC data were provided by AMPERE ( https://ampere.jhuapl.edu/ ).

Authors=Ohma, A.; Laundal, K. M.; Madelaire, M.; Hatch, S. M.; Gasparini, S.; Reistad, J. P.; Walker, S. J.; Decotte, M.;Title=Robust Estimates of Spatiotemporal Variations in the Auroral Boundaries Derived From Global UV Imaging, 2024, doi:10.1029/2023JA032021, ID:27825270.Keywords: spdf, omniSample usage ( BODY ) =The original WIC images can be accessed at https://spdf.gsfc.nasa.gov/pub/data/image/fuv/ and were processed using the FUVIEW3 software ( http://sprg.ssl.berkeley.edu/image/ ). The OMNI 1-min data is available at https://spdf.gsfc.nasa.gov/pub/data/omni/. Sample usage ( BODY ) =Solar wind plasma and magnetic field data are from the OMNI 1-min data set, time shifted to Earth’s bow shock (King Papitashvili, 2005).

Authors=Pandey, Kuldeep; Kalafatoglu Eyiguler, E. Ceren; Hussey, Glenn C.; Danskin, Donald W.; Gillies, Robert G.; Yau, Andrew W.;Title=The Ellipticity of High Frequency Transionospheric Radio Waves, 2024, doi:10.1029/2023JA032022, ID:27825273.Keywords: iri, international reference ionosphereSample usage ( BODY ) =From the International Reference Ionosphere IRI-2020 model (Bilitza et al., 2022), the peak plasma frequency over the Saskatoon radar was ~4.5 and 5 MHz during Experiment I and II, respectively. Sample usage ( BODY ) =Therefore, the background ionospheric plasma frequency would be different for these experiments.

Authors=Silveira, M. V. D.; Sibeck, D. G.; Cardoso, F. R.; Gjerloev, J. W.;Title=Tracking the Subsolar Bow Shock and Magnetopause: Applying the Magnetosheath Velocity Gradient Method, 2024, doi:10.1029/2023JA032166, ID:27825295.Keywords: cdaweb, space physics data facility, omni, omniwebSample usage ( ACK ) =The authors wholeheartedly thank NASA GSFC’s Space Physics Data Facility whose OMNIWeb Plus and CDAWeb services provided access to the solar wind, THEMIS, and UT Dallas DMSP thermal plasma observations presented in this paper. Sample usage ( BODY ) =THEMIS, Wind and DMSP data can be accessed from: https://cdaweb.gsfc.nasa.gov/. SuperMAG data can be accessed from: https://supermag.jhuapl.edu/. Sample usage ( BODY ) =The southward IMF turning seen in the OMNI data set passed THEMIS-C, D, and E from 2334 to 2336 UT with a greatly enhanced magnitude of about +50 to -50 nT. Sample usage ( BODY ) =The panels on the left side of Figure 4 show OMNIWeb Wind solar wind plasma and magnetic field observations from 2315 to 2400 UT on 14 September 2008.

Authors=Michael, A. T.; Sorathia, K. A.; Ukhorskiy, A. Y.; Albert, J.; Shen, X.; Li, W.; Merkin, V. G.;Title=Cross-Scale Modeling of Storm-Time Radiation Belt Variability, 2024, doi:10.1029/2023JA032175, ID:27825299.Keywords: cdaweb, omniSample usage ( BODY ) =The OMNI data set are available at https://cdaweb.gsfc.nasa.gov/index.html/ by selecting OMNI from the available spacecraft and then the 1-min resolution data. Sample usage ( BODY ) =The MAGE model was driven by solar wind data taken from the OMNI database at 1 min resolution. Data gaps were linearly interpolated to provide continuous boundary conditions for the simulation. The solar F10.7-cm flux index used for the ionospheric conductance was set to 124.5, the daily flux density during the event, taken from the OMNI data set. The magnetosphere simulation started at 00 UT on 17 March 2013 and was preconditioned with real solar wind for 6 hr before the sudden storm commencement.

Authors=Chen, Jia-Li; Zou, Hong; Hao, Yi-Xin; Ye, Yu-Guang; Miyoshi, Yoshizumi; Matsuoka, Ayako; Shinohara, Iku; Teramoto, Mariko; Xu, Shi-Ge;Title=A Sub-relativistic Electron Three-Belt Event in the Earth’s Radiation Belts: Observation and Explanation, 2024, doi:10.1029/2023JA032213, ID:27825320.Keywords: space physics data facility, omni, omniwebSample usage ( ACK ) =We acknowledge the Arase (ERG) team, NOAA-18 team, NASA’s Space Physics Data Facility, and SuperMAG collaboration for providing valuable data for this study. Sample usage ( BODY ) =NOAA-18 MEPED data were available from https://cdaweb.gsfc.nasa.gov/pub/data/noaa/noaa18/sem2_fluxes-2sec/2020/ provided by NASA’s Space Physics Data Facility. Interplanetary magnetic field, solar wind dynamic pressure, and solar wind velocity were provided by NASA OMNI database ( https://omniweb.gsfc.nasa.gov/ ). SME data were available from https://supermag.jhuapl.edu/mag/?.

Authors=Laskar, F. I.; Karan, D. K.; Daniell, R. E.; Codrescu, M. V.; Eastes, R. W.; Pedatella, N. M.; Wang, W.; Maute, A.; Aryal, S.; Rajesh, P. K.; McClintock, W. E.;Title=The X-Pattern Merging of the Equatorial Ionization Anomaly Crests During Geomagnetic Quiet Time, 2024, doi:10.1029/2023JA032224, ID:27825329.Keywords: spdf, space physics data facility, international reference ionosphereSample usage ( BODY ) =Data Availability Statement GOLD Level 1C NI-1 data used in this study are available at the GOLD Science Data Center ( https://gold.cs.ucf.edu/search/ ) and at NASA’s Space Physics Data Facility ( https://spdf.gsfc.nasa.gov/pub/data/gold/level1c/ ). The GIS data are available at http://formosat7.earth.ncku.edu.tw/login.php?. Sample usage ( BODY ) =It uses Gauss-Markov Kalman filter with International Reference Ionosphere (Bilitza et al., 2022) as the background model. The GIS global ionospheric data are used in several studies on ionospheric dynamical variabilities (Lin et al., 2020; Oberheide, 2022; Rajesh et al., 2021).

Authors=Engebretson, Mark J.; Gaffaney, Sean A.; Ochoa, Jesus A.; Runov, Andrei; Weygand, James M.; Nishimura, Yukitoshi; Hartinger, Michael D.; Pilipenko, Vyacheslav A.; Moldwin, Mark B.; Connors, Martin G.; Mann, Ian R.; Xu, Zhonghua; Rodriguez, Juan V.; Title=Signatures of Dipolarizing Flux Bundles in the Nightside Auroral Zone, 2024, doi:10.1029/2023JA032266, ID:27825340.Keywords: cdaweb, omni, sscwebSample usage ( BODY ) =AUTUMNX data are available from the CDAWEB site (Papitashvili King, 2020). The SuperMAG SML and SMU indices accessed in this study are available from the SuperMAG web site (Gjerloev, 2023). Sample usage ( BODY ) =Figure 3 shows IMF and solar wind data from the OMNI data base, time-shifted to the nose of the bow shock, as well as three magnetic activity indices (AL, AU, and SYM/H) from 05:20 to 06:20 UT on this day. Sample usage ( BODY ) =Candidate events on 198 days satisfied two initial criteria: they were observed during passes over the North American continent, and their ~12 R E apogees were within ~3 hr MLT of local midnight. The NASA SSCWEB utility was then used to display approximate mappings of the northern hemisphere footpoints of the magnetic field line through the relevant THEMIS spacecraft of candidate events in order to identify events that mapped to the region from west of Hudson Bay to east of Hudson Bay shown in Figure 1.

Authors=Hong, Yu; Deng, Yue; Maute, Astrid; Lu, Gang; Zhu, Qingyu; Waters, Colin; Sheng, Cheng; Lopez, Ramon; Welling, Daniel;Title=Relative Contributions of Field-Aligned Currents and Particle Precipitation to Inter-Hemispheric Asymmetry at High Latitudes During the 2015 St. Patrick’s Day Storm, 2024, doi:10.1029/2023JA032279, ID:27825343.Keywords: cdaweb, omni, omniwebSample usage ( BODY ) =IMF, solar wind and F10.7 data from the CDAWeb OMNI website were used for initializing the ionosphere and thermosphere background and pre-run conditions. Sample usage ( ACK ) =Acknowledgments This study makes use of NASA OMNI data. This work at UTA was supported by NASA through Grants 80NSSC20K1786, 80NSSC23K1062, and 80GSFC22CA011, and AFOSR through awards FA9559-16-1-0364, FA9550-23-1-0634, and FA9550-23-1-0614. The DMSP ion drift data can be obtained from http://cedar.openmadrigal.org/list.

Authors=Graham, D. B.; Khotyaintsev, Yu. V.; Dimmock, A. P.; Lalti, A.; Boldu, J. J.; Tigik, S. F.; Fuselier, S. A.;Title=Ion Dynamics Across a Low Mach Number Bow Shock, 2024, doi:10.1029/2023JA03229610.48550/arXiv.2311.11373, ID:27825355.Keywords: spdf, omniSample usage ( BODY ) =Data Availability Statement MMS data are available at https://lasp.colorado.edu/mms/sdc/public and https://spdf.gsfc.nasa.gov/pub/data/mms/. We use survey and burst mode magnetic field data from FGM (Russell et al., 2022a, 2022b), electric field data from EDP (Ergun et al., 2022). Sample usage ( BODY ) =(a-c) Solar wind and bow shock crossings. (a) Ion omni-directional energy flux. (b) Electron omni-directional energy flux.

Authors=Xia, Zhiyang; Chen, Lunjin; Horne, Richard B.; Liu, Xu; He, Jiabei; Bortnik, Jacob;Title=On the Wave-Normal Distribution of Lightning-Generated Whistlers and Their Propagation Modes, 2024, doi:10.1029/2023JA032353, ID:27825365.Keywords: spdf, space physics data facilitySample usage ( BODY ) =Data Availability Statement The data of Van Allen Probes used in this paper were provided by the Space Physics Data Facility (SPDF) https://spdf.gsfc.nasa.gov/pub/data/rbsp/.

Authors=Ajith, K. K.; Patra, A. K.; Li, Guozhu; Sripathi, S.; Pavanchaitanya, P.; Yamamoto, M.; Perwitasari, Septi;Title=Identifying the Onset Location of Equatorial Plasma Bubbles (EPBs) and Its Relationship With the Background Ionospheric Conditions, 2024, doi:10.1029/2023JA032369, ID:27825369.Keywords: cdaweb, spdfSample usage ( BODY ) =The C/NOFS CINDI-IVM data are available at NASA-SPDF ( https://cdaweb.gsfc.nasa.gov/ ) (C/NOFS, 2014).

Authors=Lozinski, Alexander R.; Horne, Richard B.; Glauert, Sarah A.; Kellerman, Adam C.; Bortnik, Jacob; Claudpierre, Seth G.; Manweiler, Jerry W.; Spence, Harlan E.;Title=Modeling Field Line Curvature Scattering Loss of 1-10 MeV Protons During Geomagnetic Storms, 2024, doi:10.1029/2023JA032377, ID:27825371.Keywords: omniSample usage ( BODY ) =A minima-finding algorithm was then applied to a time series of Dst spanning from 1983 to mid-2023, provided by NASA omni data and accessed via the Python spacepy library (Morley et al., 2011).

Authors=Zhang, Ruilong; Liu, Libo; Zhong, Jiahao; Chen, Yiding; Le, Huijun; Li, Wenbo;Title=The Middle and Low Latitude Ion Composition Variations Observed by the DMSP Satellites on 20-31 August 2018, 2024, doi:10.1029/2024JA032463, ID:27825376.Keywords: omniSample usage ( BODY ) =We use the interplanetary magnetic field Bz and SYM-H index from the OMNI data ( https://cdaweb.gsfc.nasa.gov/pub/data/**omni**/high_res_omni/ ).

Authors=Haldoupis, Christos; Haralambous, Haris; Meek, Chris;Title=A Simplified Method of True Height Analysis to Estimate the Real Height of Sporadic E Layers, 2024, doi:10.1029/2024JA032505, ID:27825379.Keywords: iri, international reference ionosphereSample usage ( BODY ) =In correspondence to the ionosonde observations, the IRI-2016 model was run to compute electron density profiles needed for the true height analysis calculations. Sample usage ( ACK ) =These include the project “International Reference Ionosphere Validation and Improvement”—IRIVIM, (Ref No: EXCELENCE/0421/0422) that was co-funded by the Republic of Cyprus and the European Regional Development Fund (ERDF), in the frame of the Operational Programme “ThAlEIA” 2021-2027 under priority 1: “Competitive, Smart and Digital Economy” and the Specific Objective (1i): “Developing and enhancing research and innovation capacities and the uptake of advanced technologies.”Sample usage ( BODY ) =To achieve this, a simple method is devised that allows the estimation of real sporadic E heights hEs from the ionosonde-measured Es parameters h ’ Es and foEs , in addition to concurrent E region electron density profiles provided by the International Reference Ionosphere empirical model IRA-2016 (Bilitza et al., 2017). Sample usage ( ABSTRACT ) =The method relies on h’ Es and foEs ionosonde measurements and E region electron density profiles obtained from the International Reference Ionosphere model. The algorithm is applied to a typical set of Digisonde observations to compute hEs and examine real height variations and functional dependencies.

Authors=Terefe, Dejene Ambisa; Nigussie, Melessew; Habarulema, John Bosco;Title=The Effect of Energy Deposition Hemispherical Asymmetry on Characteristics of LSTIDs During 17 March 2015 Geomagnetic Storm, 2024, doi:10.1029/2023JA031907, ID:28998011.Keywords: omni, omniwebSample usage ( BODY ) =Data and Method Geomagnetic Indices and Solar Wind Data The data that describe the interplanetary and geophysical conditions during space weather event of 17-18 March 2015 are obtained from OMNI Web interface. Solar wind data like solar wind speed (Vsw), and interplanetary magnetic field data, IMF, Bz, are provided by ACE Science Centre. Sample usage ( BODY ) =Data Availability Statement Solar wind parameters and geomagnetic activity indices are provided by Goddard Space Flight Center ( https://omniweb.gsfc.nasa.gov ), ACE Science Center ( http://www.srl.caltech.edu/ACE/ ), World Data Center for Geomagnetism, Kyoto ( http://wdc.kugi.kyoto-u.ac.jp ).

Authors=Atilaw, T. Y.; Akhavan-Tafti, M.; Al Shidi, Q.; Pulkkinen, T. I.; Fontaine, D.; Le Contel, O.; Slavin, J. A.; Le, G.; Chen, L. -J.; Reiff, P. H.; Alqeeq, S. W.;Title=Magnetospheric Time-History in Storm-Time Magnetic Flux Dynamics: A Global Simulation Campaign, 2024, doi:10.1029/2023JA031997, ID:28998023.Keywords: spdf, omniSample usage ( BODY ) =Data Availability Statement The magnetic field data from HSO satellites are available at the following pages, MMS: https://lasp.colorado.edu/mms/sdc/public/about/browse/mms4/fgm/srvy/l2/, Van Allen Probe: https://rbspgway.jhuapl.edu/, and GOES 15: https://spdf.gsfc.nasa.gov/pub/data/goes/goes15/. The SWMF simulation data set used in this study can be found in the University of Michigan Deep Blue repository (Al Shidi Pulkkinen, 2023).Sample usage ( BODY ) =The simulated SYM-H starts to diverge from OMNI data during the storm main phase, the difference becomes ~75 nT at around 08 UT on 20 Dec 2015 (see Figure 1a).

Authors=Shi, Yining; Moldwin, Mark B.;Title=Non-Geophysical Interhemispheric Asymmetries in Large Magnetic Field Residuals Between Swarm Observations and Earth Magnetic Field Models During Moderate to Quiet Geomagnetic Conditions, 2024, doi:10.1029/2023JA032092, ID:28998028.Keywords: space physics data facility, omni, omniwebSample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s OMNIWeb service, and OMNI data https://omniweb.gsfc.nasa.gov/. Sample usage ( BODY ) =Figure 1b has 50% of large residuals in NH and 55% in SH occurring during AE 500 nT but note that 10% of AE indices are missing as provided by NASA/GSFC’s OMNI data set through OMNIWeb (Papitashvili King, 2020). AE index appears to show higher level of geomagnetic activity level than Dst and Kp indices, which is expected since Figure 1c shows that all large residuals appear in the high latitude region. AE index appears to show higher level of geomagnetic activity level than Dst and Kp indices, which is expected since Figure 1c shows that all large residuals appear in the high latitude region.

Authors=Hull, Arthur J.; Muschietti, Laurent; Agapitov, Oleksiy V.; Chaston, Christopher C.; Le Contel, Olivier; Lindqvist, Per-Arne;Title=Energy Transport and Conversion Within Earth’s Supercritical Bow Shock: The Role of Intense Lower-Hybrid Whistler Waves, 2024, doi:10.1029/2023JA031630, ID:28998043.Keywords: omni, omniwebSample usage ( BODY ) =Data Availability Statement The MMS data used in this study are publicly available at the MMS Science Data Center website https://lasp.colorado.edu/mms/sdc/public/. OMNI upstream solar wind pressures are available from https://omniweb.gsfc.nasa.gov/. Sample usage ( BODY ) =Both events reported by Sundkvist et al. ( 2012) are associated with low values for the solar wind dynamic pressure (obtained from OMNIWEB), with P SW ~ 2.4 nPa and P SW ~ 1.9 nPa for the first and second event, respectively.

Authors=Pradipta, Rezy; Huang, Chaosong; Groves, Keith M.;Title=A 2-Dimensional Data Detrending Technique for Equatorial Plasma Bubble Studies Using GOLD Far Ultraviolet Observations, 2024, doi:10.1029/2023JA031963, ID:28998047. Keywords: spdf, space physics data facility, iriSample usage ( BODY ) =Data Availability Statement The NASA GOLD Level 1C observation datafiles for this study are available from the GOLD mission webpage at https://gold.cs.ucf.edu/data/ or from the NASA Space Physics Data Facility webpage at https://spdf.gsfc.nasa.gov/pub/data/gold/level1c/. Sample usage ( BODY ) =(b) The process will no longer be only about the relative level of depletions, but the end result is going to be expressed in terms of ionospheric plasma density and/or TEC values. (3) The background plasma density and/or TEC may be obtained from ionosphere models such as IRI, NeQuick, NET, TIE-GCM, or WAM-IPE (Bilitza et al., 2022; Coisson et al., 2006; Fang et al., 2018; Nava et al., 2008; Qian et al., 2014; Smirnov et al., 2023).

Authors=Feng, Huiting; Wang, Dedong; Guo, Deyu; Shprits, Yuri Y.; Han, Desheng; Teng, Shangchun; Ni, BinBin; Shi, Run; Zhang, Yongliang;Title=Lower Band Chorus Wave Scattering Causing the Extensive Morningside Diffuse Auroral Precipitation During Active Geomagnetic Conditions: A Detailed Case Study, 2024, doi:10.1029/2023JA032240, ID:28998092.Keywords: cdaweb, space physics data facility, omniSample usage ( BODY ) =We acknowledge the use of NASA/GSFC’s Space Physics Data Facility’s OMNI Web service at https://cdaweb.gsfc.nasa.gov/index.html . The Kp index was provided by GFZ Section 2.3 and downloaded from the World Data Center. Sample usage ( BODY ) =The interplanetary magnetic field data used in this study are extracted from the National Aeronautics and Space Administration/Goddard Space Flight Center (NASA/GSFC)‘s OMNI data set. Conjugate Measurement of Morningside Diffuse Aurora and In Situ Wave Observations on 1 January 2016 We report a morningside diffuse aurora event associated with chorus wave activity, jointly observed by the DMSP and RBSP-B on 1 January 2016 during the recovery phase of a substorm. Figures 1a and 1b show the solar wind dynamic pressure and geomagnetic indices from 0700 UT to 1100 UT derived from OMNI 1-min data. During this period, the geomagnetic condition is relatively active, accompanied by substorm events (Kp index changes from 5 to 3, not shown here).

Authors=Zou, Wenqian; Li, Haimeng; Hu, Peng; Wang, Dedong; Tang, Rongxin; Ouyang, Zhihai; Yuan, An; Feng, Bopu; Deng, Xiaohua;Title=Statistical Properties of Exohiss Waves and Associated Scattering Losses of Radiation Belt Electrons, 2024, doi:10.1029/2023JA032244, ID:28998096.Keywords: spdfSample usage ( BODY ) =The Van Allen Probes data used in this study are available from https://spdf.gsfc.nasa.gov/pub/data/rbsp/.

Authors=Kim, K. -H.; Jun, C. -W.; Kwon, J. -W.; Lee, J.; Shiokawa, K.; Miyoshi, Y.; Kim, E. -H.; Min, K.; Seough, J.; Asamura, K.; Shinohara, I.; Matsuoka, A.; Yokota, S.; Kasahara, Y.; Kasahara, S.; Hori, T.; Keika, K.; Kumamoto, A.; Tsuchiya, F.;Title=Observation and Numerical Simulation of Cold Ions Energized by EMIC Waves, 2024, doi:10.1029/2023JA032361, ID:28998111.Keywords: omni, omniwebSample usage ( BODY ) =Solar wind data (solar wind velocity and density) used in this study are available in the NASA OMNI database ( https://omniweb.gsfc.nasa.gov ). The OMNI data were provided in 1 min resolution.

Authors=Zhang, Kedeng; Wang, Hui; Liu, Jing;Title=The Short-Periodic Response of Equatorial Electrojet to the Temporal Variations of IMF Bz During Geomagnetic Quiet Time, 2024, doi:10.1029/2023JA032197, ID:28998116.Keywords: omniSample usage ( BODY ) =In this study, the high-latitude electric field in TIEGCM is specified by the empirical Weimer model, with solar wind data from OMNI input. The solar wind data has a resolution of 1 min. The timestep of TIEGCM is 30 s.

Authors=Vu, Andrew; Liu, Terry Z.; Angelopoulos, Vassilis; Zhang, Hui;Title=2.5-D Local Hybrid Simulations of Discontinuity-Driven Compressional Boundaries Under Various Magnetic Field Geometries, 2024, doi:10.1029/2023JA032302, ID:28998122.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement The simulation data output that was used for the figures and analysis in this study is available at (Vu, 2023a, 2023b). THEMIS data are available at CDAWeb ( https://cdaweb.gsfc.nasa.gov/ ).

Authors=Ashok, Arya; Ambili, K. M.; Choudhary, R. K.;Title=A Numerical Study on the Impact of E x B Drift on the Vertical Distribution of the Plasma Density Over the Geomagnetic Equatorial Ionospheric Region, 2024, doi:10.1029/2024JA032589, ID:28998123.Keywords: iri, international reference ionosphereSample usage ( ACK ) =The authors gratefully acknowledge MSIS ( https://ccmc.gsfc.nasa.gov/models/NRLMSIS~00/ ) and IRI ( https://ccmc.gsfc.nasa.gov/models/**IRI**~2016/ ) for the neutral density and temperature data sets used in the study. Solar flux in the range 0.5-189.5 nm is obtained from the Solar EUV Experiment (SEE) instrument onboard the NASA Thermosphere Ionosphere Energetics and Dynamics (TIMED) mission ( https://lasp.colorado.edu/see/data/ ). Sample usage ( BODY ) =The electron and the ion temperatures are obtained from the International Reference Ionosphere (IRI) model ( https://ccmc.gsfc.nasa.gov/models/**IRI**~2016/ ).

Authors=Zhang, Kedeng; Wang, Hui; Song, Huimin; Zhong, Yunfang; Xia, Hao; Sun, Yu; Wang, Chengzhi;Title=The Seasonal Dependence of the Unexpected Afternoon Westward Equatorial Electrojet During Quiet Time, 2024, doi:10.1029/2023JA032372, ID:28998128.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement The CNOFS observed E x B drifts and AE index can be downloaded at Coordinated Data Analysis Web ( https://cdaweb.gsfc.nasa.gov/istp_public/ ). The results presented in this paper rely on the data collected at Tir and Abg ( https://supermag.jhuapl.edu ), following Download Data-Large Downloads-Prepacked NetCDF files (Search TIR and ABG).

Authors=Yin, Ze-Fan; Zhou, Xu-Zhi; Hu, Ze-Jun; Yue, Chao; Zong, Qiu-Gang; Liu, Zhi-Yang; Liu, Jian-Jun; Shiokawa, Kazuo; Oyama, Shin-ichiro; Baishev, Dmitry;Title=Westward Excursion of Pc1/EMIC Waves and Their Source Protons: Paradoxical Observations From Ground and Space, 2024, doi:10.1029/2023JA032317, ID:28998137.Keywords: omni, omniwebSample usage ( BODY ) =The AU/AL indices are available at OMNI Web ( https://omniweb.gsfc.nasa.gov/ ).Sample usage ( BODY ) =The AU/AL indices are available at OMNI Web ( https://omniweb.gsfc.nasa.gov/ ).

Authors=Lu, Xi; Otto, Antonius; Zhang, Hui; Liu, Terry; Chen, Xingran;Title=The Bow Shock and Magnetosheath Responses to Density Depletion Structures, 2024, doi:10.1029/2024JA032566, ID:28998145.Keywords: cdaweb, omniSample usage ( BODY ) =ACE, WIND, and OMNI data are available at NASA’s Coordinated Data Analysis Web (CDAWeb, https://cdaweb.gsfc.nasa.gov ). The simulation model is from Otto Zhang, 2021.Sample usage ( BODY ) =Solar wind conditions are obtained from the OMNI 1-min resolution data. The selection criteria for the observation cases are listed as follow.

Authors=Ghaly, F.; Spanswick, E.; Gillies, R.; Cameron, T.; Skone, S.; Fiori, R. A. D.; Weatherwax, A. T.;Title=Use of Terrestrial High Frequency Signals in Riometer Data to Explore the Size of D-Region Electron Density Enhancements, 2024, doi:10.1029/2023JA032375, ID:28998146.Keywords: iri, international reference ionosphereSample usage ( BODY ) =Utilizing electron density profiles from the International Reference Ionosphere model (IRI) (Fron et al., 2020) and the Provision of High-Frequency Raytracing Laboratory for Propagation Studies (PHaRLAP) toolbox, we simulate the pre-event raypath that facilitated signal reception by the riometer.

Authors=Ma, Wenqing; Zhou, Meng; Zhong, Zhihong; Deng, Xiaohua;Title=Quantitative Analysis of Electron Heating and Acceleration in Coalescing Magnetic Flux Ropes at Earth’s Magnetopause, 2024, doi:10.1029/2023JA032270, ID:28998153.Keywords: omniSample usage ( BODY ) =From the top to bottom are: (a) magnetic field vectors; (b) magnetic field strength; (c) plasma density; (d) ion bulk velocity; (e) electron bulk velocity; (f) ion and (g) electron omni-directional differential energy fluxes. All vectors are presented in GSM coordinates.

Authors=Trattner, K. J.; Fuselier, S. A.; Kletzing, C. A.; Bonnell, J. W.; Bounds, S. R.; Petrinec, S. M.; Sawyer, R. P.; Yeoman, T. K.; Ergun, R. E.; Burch, J. L.;Title=TRICE-2/SuperDARN Observations and Comparison With the Associated MMS Magnetopause Crossing, 2024, doi:10.1029/2023JA032263, ID:28998165.Keywords: cdawebSample usage ( BODY ) =The solar wind data are available at CDAWeb ( http://cdaweb.gsfc.nasa.gov/istp_public/ ). The study also uses data from a long-standing global network known as the Super Dual Auroral Radar Network (SuperDARN) (e.g., Chisham et al., 2007; Greenwald et al., 1995; Nishitani et al., 2019).

Authors=Sun, Meng; Lu, Jianyong; Li, Jingyuan; Tang, Fen; Wei, Guanchun; Li, Zheng; Yue, Fulu; Xiong, Shiping; Huang, Ningtao;Title=Responses of Mesosphere Temperature to the Geomagnetic Storms on 8 and 15 September 2003, 2024, doi:10.1029/2023JA032366, ID:28998169.Keywords: omni, omniwebSample usage ( BODY ) =The IMF B y and B z , solar wind speed, SYM-H, and AE indices are obtained from the OMNI database ( https://omniweb.gsfc.nasa.gov/ ). The Kp index is provided by the CelesTrak website ( http://www.celestrak.com/SpaceData/SW-All.txt ). Sample usage ( BODY ) =The IMF B y and B z , solar wind speed, SYM-H, and AE indices are obtained from the OMNI database ( https://omniweb.gsfc.nasa.gov/ ). The Kp index is provided by the CelesTrak website ( http://www.celestrak.com/SpaceData/SW-All.txt ).

Authors=Lee, S. H.; Sibeck, D. G.; Weimer, D. R.; Omidi, N.;Title=Orientation of IMF Discontinuity Normals Across the Solar Cycles, 2024, doi:10.1029/2023JA032329, ID:28998170.Keywords: cdawebSample usage ( BODY ) =We use 16-s time resolution level 2 ACE IMF observations acquired by MAG (Smith et al., 1998) and 64-s resolution solar wind ion data obtained by SWEPAM (Solar Wind Electron Proton Alpha Monitor) (McComas et al., 1998) from CDAWeb ( cdaweb.gsfc.nasa.gov ). We choose to study the years of 2001, 2002, 2012, and 2014 (representative of solar maximum periods during solar cycles 23 and 24) and 2008, 2009, 2019, and 2020 (representative of solar minimum) to conduct this study.

Authors=Liu, Terry Zixu; Angelopoulos, Vassilis; Zhang, Hui; Vu, Andrew; Raeder, Joachim;Title=Magnetosheath Ion Field-Aligned Asymmetry and Implications for Ion Leakage to the Foreshock, 2024, doi:10.1029/2023JA03233910.48550/arXiv.2402.01978, ID:28998175. Keywords: cdaweb, omniSample usage ( BODY ) =Data Availability Statement Time History of Events and Macroscale Interactions during Substorms mission data set and OMNI data set are available at NASA’s Coordinated Data Analysis Web (CDAWeb, http://cdaweb.gsfc.nasa.gov/ ). Magnetospheric Multiscale data set is available at https://lasp.colorado.edu/mms/sdc/public/. Sample usage ( BODY ) =We analyze plasma data from the MMS fast plasma investigation (FPI) instrument suite (Pollock et al., 2016) and the THEMIS electrostatic analyzer (ESA) (McFadden et al., 2008) and DC magnetic field data from the MMS fluxgate magnetometer (Russell et al., 2016) and the THEMIS fluxgate magnetometer (Auster et al., 2008). We use OMNI data to determine the upstream conditions. With OMNI as input, the Open GGCM model is used to demonstrate global magnetic field geometry.

Authors=Oliveira, Denny M.; Zesta, Eftyhia;Title=Inter-Hemispheric Energy Input Into the Ionosphere-Thermosphere System During Magnetic Storms: What We Can and Cannot Learn From DMSP Observations, 2024, doi:10.1029/2024JA032486, ID:28998178.Keywords: omni, omniwebSample usage ( BODY ) =IMF and Magnetic Index Data NASA’s OMNI IMF data are used in this study (King Papitashvili, 2005). IMF data, with time resolution of 1 min, is shifted from L1 to the magnetopause nose ( X ~ 17 Earth’s radii) as described by King and Papitashvili ( 2005). Sample usage ( BODY ) =The NASA OMNI database is available online at https://omniweb.gsfc.nasa.gov. The SYM-H data is located at the website http://wdc.kugi.kyoto-u.ac.jp and described in World Data Center for Geomagnetism, Kyoto et al. ( 2022).

Authors=Regoli, L. H.; Gkioulidou, M.; Ohtani, S.; Raptis, S.; Mouikis, C. G.; Kistler, L. M.; Cohen, I. J.; Fuselier, S. A.;Title=Temporal Evolution of O+ Population in the Near-Earth Plasma Sheet During Geomagnetic Storms as Observed by the Magnetospheric Multiscale Mission, 2024, doi:10.1029/2023JA032203, ID:28998182.Keywords: omni, omniwebSample usage ( BODY ) =Figure 1 shows data from the MMS 1 spacecraft and the SYM-H index obtained from the OMNI dataset (panel a) during a storm that took place in July 2017. This event corresponds to one of the storms included in the statistical analysis presented in the next section, where O + access is observed in the near-Earth plasma sheet. Sample usage ( BODY ) =Instrumentation In order to understand the temporal evolution of O + ions during geomagnetic storms, we use data from the Hot Plasma Composition Analyzer (HPCA, Young et al., 2016) onboard the MMS 1 spacecraft, as well as the SYM-H index provided by OMNIWeb. The SYM-H index is derived by subtracting the geomagnetic field and solar quiet variation from the data obtained by six ground-based magnetic stations.

Authors=Kuai, Jiawei; Sun, Hao; Liu, Libo; Zhong, Jiahao; Yue, Xinan; Wang, Kang; Zhang, Ruilong; Li, Qiaoling; Yang, Yuyan; Jin, Yihong; Dong, Yi; Wan, Xin; Chen, Jiawen;Title=A Case Study of Ionospheric Storm-Time Altitudinal Differences at Low Latitudes During the May 2021 Geomagnetic Storm, 2024, doi:10.1029/2024JA032484, ID:28998187. Keywords: cdaweb, omniwebSample usage ( BODY ) =The ICON data is available at the website of https://cdaweb.gsfc.nasa.gov/pub/data/icon/. We are also grateful to the broader ICON team. Sample usage ( BODY ) =Data Availability Statement The solar wind data are obtained from the OMNIWeb interface at http://omniweb.gsfc.nasa.gov. GPS TEC data are provided by the MIT Haystack Observatory Madrigal database (http://madrigal.haystack.edu/madrigal/).

Authors=Schmolter, Erik; Duhnen, Hanna; Berdermann, Jens; Vaishnav, Rajesh; Jacobi, Christoph;Title=Spatial Features of the Delayed Ionospheric Response During Low and High Solar Activity, 2024, doi:10.1029/2024JA032672, ID:28998188.Keywords: spdf, omni, omniwebSample usage ( BODY ) =Data Availability Statement OMNI data were obtained from the GSFC/SPDF OMNIWeb interface at https://omniweb.gsfc.nasa.gov/. SDO/EVE data were obtained from the LASP web interface at https://lasp.colorado.edu/eve/data/. Sample usage ( BODY ) =Both data sets are also included in the National Aeronautics and Space Administration (NASA) Goddard Space Flight Center’s (GSFC) OMNI database, that can be accessed through the OMNIWeb interface (NASA, 2023). Solar Spectral EUV Irradiance The Extreme ultraviolet Variability Experiment (EVE) of the Solar Dynamics Observatory (SDO) missions measures the solar irradiance (Didkovsky et al., 2009; Hock et al., 2010; Pesnell et al., 2011; Woods et al., 2010) with two Multiple EUV Grating Spectrographs (MEGS) from 6 to 17 nm (A), from 17 to 37 nm (A) and from 37 to 106 nm (B).

Authors=Beyene, F.; Angelopoulos, V.;Title=Storm-Time Very-Near-Earth Magnetotail Reconnection: A Statistical Perspective, 2024, doi:10.1029/2024JA032434, ID:28998193.Keywords: cdaweb, spdf, space physics data facility, omni, omniwebSample usage ( ACK ) =We thank the SPEDAS software team and NASA’s Coordinated Data Analysis Web (CDAWeb, https://cdaweb.gsfc.nasa.gov/ ) for their analysis tools and data access.Sample usage ( BODY ) =The OMNI data, including solar wind parameters and geomagnetic indices, were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. THEMIS mission data and OMNI data have been imported and analyzed using corresponding plug-ins to the SPEDAS analysis platform ( http://spedas.org Angelopoulos et al., 2019). Sample usage ( BODY ) =To study the solar wind magnetic field and dynamic pressure conditions during these events, we use 1-min resolution solar wind magnetic field and plasma data from ACE, WIND, and IMP, time-shifted to the magnetopause nose, combined into the OMNI Data set by, and available at, the Space Physics Data Facility. To put the VNERX events into the context of ring current energization and ionospheric dissipation we use the Symmetric H (SYM-H) and Auroral Electrojet (AE) indices from the World Data Center for Geomagnetism, Kyoto (WDC-Kyoto). Sample usage ( BODY ) =(a) Auroral Electrojet (AE) index from the OMNI data set. (b) Symmetric H (SYM-H) index from the OMNI data set. Sample usage ( BODY ) =The OMNI data, including solar wind parameters and geomagnetic indices, were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov. THEMIS mission data and OMNI data have been imported and analyzed using corresponding plug-ins to the SPEDAS analysis platform ( http://spedas.org Angelopoulos et al., 2019).

Authors=Barad, Rajesh Kumar; Sripathi, S.; Banola, S.; Vijaykumar, K.;Title=Occurrence of Equatorial Plasma Bubbles (EPBs) Over the Indian Region on 15 January 2022 and Their Plausible Connection to the Tonga Volcano Eruption, 2024, doi:10.1029/2023JA031542, ID:29097213.Keywords: spdf, omni, omniwebSample usage ( BODY ) =ICON-IVM/MIGHTI data are available at https://icon.ssl.berkeley.edu/Data and https://spdf.gsfc.nasa.gov/. GPS-TEC data can be accessed at https://cddis.nasa.gov/Data and http://madrigal.haystack.mit.edu/madrigal/. Sample usage ( BODY ) =Data Availability Statement Visit https://omniweb.gsfc.nasa.gov/form/omni_min.html to access OMNI data. The geomagnetic activity indices are available online at http://wdc.kugi.kyoto-u.ac.jp/.

Authors=Babu, S. S.; Mann, I. R.; Donovan, E. F.; Smith, A. W.; Dimitrakoudis, S.; Sydora, R. D.; Kale, A.;Title=Plasma Sheet Counterparts for Auroral Beads and Vortices in Advance of Fast Flows: New Evidence for Near-Earth Substorm Onset, 2024, doi:10.1029/2023JA031957, ID:29097215.Keywords: omniSample usage ( BODY ) =The last two panels show the solar wind velocity (in GSE) and the proton density from OMNI and from the time-shifted Wind and DSCOVR data (See text for details). The solar wind data provided by OMNI was taken from the time-shifted Wind data projected to the bow shock nose (BSN) location.

Authors=Wu, Qian; Wang, Wenbin; Lin, Dong; Qian, Liying; Huang, Chaosong; Zhang, Yongliang;Title=MAGE Model Simulation of the Pre-Reversal Enhancement and Comparison With ICON and Jicamarca ISR Observations, 2024, doi:10.1029/2023JA032038, ID:29097217. Keywords: cdaweb, omniSample usage ( BODY ) =The simulation used in this study is driven by CDAWeb OMNI database with one-minute resolution. The TIEGCM is set with 1.25deg latitudinal and longitudinal resolution with 0.25 scale height. Sample usage ( BODY ) =The simulation used in this study is driven by CDAWeb OMNI database with one-minute resolution. The TIEGCM is set with 1.25deg latitudinal and longitudinal resolution with 0.25 scale height.

Authors=Wang, Xiaochuan; Lei, Jiuhou; Zhang, Shun-Rong; Li, Zezhong; Dang, Tong; Luan, Xiaoli; Dou, Xiankang;Title=Simulation of Nighttime Medium-Scale Traveling Ionospheric Disturbances in the Midlatitude Ionosphere During Stormtime, 2024, doi:10.1029/2023JA032051, ID:29097218.Keywords: omni, omniwebSample usage ( BODY ) =Solar wind and geomagnetic index data can be found from NASA OMNIWeb https://omniweb.gsfc.nasa.gov/form/omni_min.html. Millstone Hill Hi-Res FPI data can be downloaded from Madrigal:. Sample usage ( BODY ) =Solar wind and geomagnetic index data can be found from NASA OMNIWeb https://omniweb.gsfc.nasa.gov/form/omni_min.html. Millstone Hill Hi-Res FPI data can be downloaded from Madrigal:.

Authors=Nose, Masahito; Hosokawa, Keisuke; Nomura, Reiko; Teramoto, Mariko; Asamura, Kazushi; Miyoshi, Yoshizumi; Mitani, Takefumi; Sakanoi, Takeshi; Namekawa, Taku; Kawano, Takeshi; Iwanaga, Yoshihiro; Tatematsu, Shunichi; Hirahara, Masafumi; Halford, Alexa; Shumko, Mykhaylo; Lessard, Marc R.; Lynch, Kristina; Paschalidis, Nicholaos; Jaynes, Allison N.; McHarg, Matthew G.;Title=Field-Aligned Currents Associated With Pulsating Auroral Patches: Observation With Magneto-Impedance Magnetometer (MIM) Onboard Loss Through Auroral Microburst Pulsations (LAMP) Sounding Rocket, 2024, doi:10.1029/2023JA032232, ID:29097221.Keywords: omniSample usage ( BODY ) =For E b, the value of 10 mV/m is taken from a recent empirical model for the high-latitude electric field (ASHLEY-E) developed by Zhu et al. ( 2021) at 00 MLT and 66deg GMLAT with the OMNI data at 10 UT on 5 March 2022 (IMF B y = 0.2 nT, IMF B z = -3.5 nT, V SW = 448 km/s, and N SW = 8.5 cm -3 ).

Authors=Glauert, S. A.; Atkinson, J. W.; Ross, J. P.; Horne, R. B.;Title=A New Model of Electron Pitch Angle Distributions and Loss Timescales in the Earth’s Radiation Belts, 2024, doi:10.1029/2023JA032249, ID:29097222.Keywords: omni, omniwebSample usage ( BODY ) =The distributions are required to map Low Earth Orbit (LEO) electron flux observations from the observed low equatorial pitch angles to the magnetic equator, and for deriving pitch angle distributions from omni-directional observations, such as those provided by GPS satellites. Sample usage ( BODY ) =Data Availability Statement The Kp index was provided by OMNIWeb ( https://omniweb.gsfc.nasa.gov ). The diffusion coefficients, loss timescales and pitch angle distributions reported in this paper are available from the NERC EDS UK Polar Data Centre ( https://doi.org/10.5285/6d20ed7b-59e1-4284-a6f2-3e2589da6d2a ).

Authors=Shreedevi, P. R.; Yu, Yiqun; Miyoshi, Yoshizumi; Tian, Xingbin; Zhu, Minghui; Jordanova, Vania K.; Nakamura, Satoko; Jun, Chae-Woo; Kumar, Sandeep; Shiokawa, Kazuo; Connors, Martin; Hori, T.; Shoji, Masafumi; Shinohara, I.; Yokota, S.; Kasahara, S.; Keika, K.; Matsuoka, A.; Kadokura, Akira; Tsuchiya, Fuminori; Kumamoto, Atsushi; Kasahara, Yoshiya;Title=Global Distribution of EMIC Waves and Its Association to Subauroral Proton Precipitation During the 27 May 2017 Storm: Modeling and Multipoint Observations, 2024, doi:10.1029/2023JA032337, ID:29097225. Keywords: cdaweb, omniwebSample usage ( BODY ) =Solar wind and geomagnetic indices are provided by http://cdaweb.gsfc.nasa.gov. National Oceanic and Atmospheric Administration MetOp data and the DMSP data are available at http://satdat.ngdc.noaa.gov/sem/poes/ and http://www.ngdc.noaa.gov/stp/satellite/dmsp/. Sample usage ( BODY ) =These data are available from the OMNIWeb database and the World Data Center, Kyoto, respectively. The particle precipitation into the ionosphere is studied using the in situ measurements from the DMSP and the NOAA Meteorological Operational satellite (MetOp) 01 and 02 satellites.

Authors=Barani, Mohammad; Poppe, Andrew R.; Fillingim, Matt O.; McFadden, J. P.; Halekas, J. S.; Sibeck, David G.;Title=A Study of Ionospheric Heavy Ions in the Terrestrial Magnetotail Using ARTEMIS, 2024, doi:10.1029/2023JA032346, ID:29097227. Keywords: cdaweb, spdf, space physics data facility, omniSample usage ( BODY ) =ARTEMIS data are available at Coordinated Data Analysis Web (CDAWeb) (https://cdaweb.gsfc.nasa.gov/cgi-bin/eval1.cgi) in the NASA’s Space Physics Data Facility (SPDF) platform of GSFC. Sample usage ( BODY ) =For each ARTEMIS observation, we also retrieved the upstream solar wind parameters and geomagnetic activity indices via the NASA/OMNI data set (King Papitashvili, 2005). The OMNI data were shifted by 40 min with respect to the times heavy ions were observed at the tail since it takes approximately this long for ions to reach lunar distances within the downstream magnetotail after the solar wind encounters the sub-solar magnetopause.

Authors=Imtiaz, Nadia; Dugassa, Teshome; Calabia, Andres; Anoruo, Chukwuma; Kashcheyev, Anton;Title=Westward PPEF Plays Important Role in the Suppression of Post-Midnight Plasma Irregularities: A Case Study of the November 2021 Geomagnetic Storm, 2024, doi:10.1029/2023JA032367, ID:29097229. Keywords: spdf, omni, omniwebSample usage (ACK) =Acknowledgments We acknowledge to the SPDF OMNIWeb database as the source of OMNI data. The geomagnetic indices calculated and made available by ISGI Collaborating Institutes from data collected at magnetic observatories. Sample usage (BODY) =Data Availability Statement Data: Solar wind parameters are obtained from the GSFC/SPDF OMNIWeb interface (https://omniweb.gsfc.nasa.gov/form/omni_min.html) and geomagnetic indices from ISGI (https://isgi.unistra.fr/data_download.php). Sample usage (ACK) =Acknowledgments We acknowledge to the SPDF OMNIWeb database as the source of OMNI data. The geomagnetic indices calculated and made available by ISGI Collaborating Institutes from data collected at magnetic observatories. Sample usage ( BODY ) =The data is available at the NASA’s OMNIWeb database https://omniweb.gsfc.nasa.gov/form/omni_min.html (King Papitashvili, 2005). The global TEC maps, updated every 5 min, are available in Coupling, Energetics, and Dynamics of Atmospheric Regions (CEDAR) Madrigal database.

Authors=da Silva, D. E.; Elkington, S. R.; Li, X.; Murphy, J.; Hudson, M. K.; Wiltberger, M. J.; Chan, A. A.;Title=Numerical Calculations of Adiabatic Invariants From MHD-Driven Magnetic Fields, 2024, doi:10.1029/2023JA032397, ID:29097232. Keywords: spdf, space physics data facility, omni, omniwebSample usage ( BODY ) =Data from the OMNI database is available from OMNIWeb and NASA Goddard Spaceflight Center (GSFC) Space Physics Data Facility (SPDF) at https://omniweb.gsfc.nasa.gov/. Data from the GOES13 magnetometers is available online from the National Centers for Environmental Information (NCEI) at https://www.ngdc.noaa.gov/stp/satellite/goes/. Data from the GOES13 magnetometers is available online from the National Centers for Environmental Information (NCEI) at https://www.ngdc.noaa.gov/stp/satellite/goes/. Sample usage ( BODY ) =Finally, in Figure 7 we see L * calculated at increasing distances into the tail and two mirroring magnetic latitudes (15deg and 30deg). The OMNI IMF parameters during this storm are provided in Appendix A. The most variation in L * over the course of the storm occurs at larger distances into the tail, where the influence of the external field over the dipole is the greatest. Sample usage ( BODY ) =This data was taken from the OMNI database ( https://omniweb.gsfc.nasa.gov/ ). The CME-driven enhancement associated with abrupt increases in IMF number density and velocity occurs around 2 October at 06:00.

Authors=Evans, J. S.; Lumpe, J. D.; Eastes, R. W.; Correira, J.; Aryal, S.; Laskar, F.; Veibell, V.; Krywonos, A.; Plummer, T.; McClintock, W. E.;Title=Disk Images of Neutral Temperature From the Global-Scale Observations of the Limb and Disk (GOLD) Mission, 2024, doi:10.1029/2024JA032424, ID:29097234.Keywords: spdf, space physics data facilitySample usage ( BODY ) =Data Availability Statement Global-scale Observations of the Limb and Disk (GOLD) Level 1C DAY and Level 2 TDISK data used in this paper can be obtained at the GOLD website, https://gold.cs.ucf.edu/search/, and NASA’s Space Physics Data Facility (SPDF), https://spdf.gsfc.nasa.gov/pub/data/gold/. To access data through the University of Central Florida website, enter the start and end dates in the pull down menu, select “Level 1C - Day” for Level 1C DAY data, or “Level 2 - TDISK” for TDISK data, and click the “Search” button.

Authors=Ouyang, Xin-Yan; Yue, Chao; Wang, Yong-Fu; Ren, Jie; Yang, Mu-Ping; Wang, Ya-Lu; Wu, Ying-Yan; Zhang, Xue-Min;Title=Revealing the EMIC Wave Frequency Differences in the Ionosphere via Coordinated Observations: A Case Study, 2024, doi:10.1029/2024JA032425, ID:29097235.Keywords: space physics data facilitySample usage ( ACK ) =We are grateful to NASA/GSFC’s Space Physics Data Facility, ERG science center, Swarm team, CSES team, and ISEE induction magnetometer/PWING project team for data.

Authors=Ma, Yu-Zhang; Zhang, Qing-He; Zhao, Si-Han; Lyons, Larry R.; Oksavik, Kjellmar; Xing, Zan-Yang; Wang, Yong; Hairston, Marc R.; Liu, Jian-Jun; Nanan, Balan; Deng, Zhong-Xin; Zhang, Qiang;Title=Multi-Instrument Analysis of the Formation and Segmentation of Tongue of Ionization Into Two Consecutive Polar Cap Patches, 2024, doi:10.1029/2024JA032426, ID:29097236.Keywords: omni, omniwebSample usage ( BODY ) =Observations Interplanetary Magnetic Field and Solar Parameters Figures 1a-1c show the interplanetary magnetic field (IMF) and solar wind parameters from OMNI. The OMNI data has been lagged by 6-min for the propagation delay from the nose of bow shock to the dayside ionosphere (Figure S2 in Supporting Information S1). Sample usage ( BODY ) =The OMNI data is obtained from OMNIWeb ( https://omniweb.gsfc.nasa.gov/ow_min.html ).

Authors=Sun, Wenjie; Li, Guozhu; Zhang, Shun-Rong; Hu, Lianhuan; Dai, Guofeng; Zhao, Biqiang; Otsuka, Yuichi; Zhao, Xiukuan; Xie, Haiyong; Li, Yi; Ning, Baiqi; Liu, Libo; Shinbori, Atsuki; Nishioka, Michi; Perwitasari, Septi;Title=Regional Ionospheric Super Bubble Induced by Significant Upward Plasma Drift During the 1 December 2023 Geomagnetic Storm, 2024, doi:10.1029/2024JA032430, ID:29097237.Keywords: omni, omniwebSample usage ( BODY ) =We retrieved the main parameters of these super EPBs based on the published OMNI data and the global grid ROTI product, which are listed in Table 1. Sample usage ( BODY ) =The auroral electrojet (AE) index reproduced from the online quick-look plots ( https://wdc.kugi.kyoto-u.ac.jp/ae_realtime/ ), solar wind speed, and interplanetary magnetic field (IMF) Bz component ( https://omniweb.gsfc.nasa.gov/ow.html/ ) were used to investigate possible driving forces for the EPB generation during the geomagnetic storm.

Authors=Toy-Edens, Vicki; Mo, Wenli; Raptis, Savvas; Turner, Drew L.;Title=Classifying 8 Years of MMS Dayside Plasma Regions via Unsupervised Machine Learning, 2024, doi:10.1029/2024JA032431, ID:29097238.Keywords: omni, heliocloudSample usage ( BODY ) =DIS consisted of 32 channels ranging from 10 eV to 30 keV with a temporal resolution of 150 ms. We used the ion omni-directional flux and temperature from the DIS fast survey moments data set which was reported on an integrated 4.5 s time cadence. Sample usage ( ACK ) =We used tools created by the HelioCloud Project. The authors thank the numerous individuals who supported to the MMS mission and made the data available. Sample usage ( BODY ) =We perform this analysis on the Amazon Web Services (AWS) cloud using the Heliocloud framework (Thomas et al., 2022), which provided computational tools and cloud object storage of MMS data.

Authors=Simms, L. E.; Ganushkina, N. Y.; Dubyagin, S.;Title=Comparing Influences of Solar Wind, ULF Waves, and Substorms on 20 eV-2 MeV Electron Flux (RBSP) Using ARMAX Models, 2024, doi:10.1029/2024JA032458, ID:29097240.Keywords: omniwebSample usage ( BODY ) =Solar wind and IMF parameters as well as geomagnetic indices (Kp index and SymH), were obtained from OMNIWeb with data time-shifted to the bow shock nose: https://omniweb.gsfc.nasa.gov/form/dx1.html.

Authors=Sibeck, D. G.; Lee, S. -H.;Title=A Pressure Pulse-Driven Transient Magnetospheric Event, 2024, doi:10.1029/2024JA032468, ID:29097241.Keywords: cdaweb, sscwebSample usage ( BODY ) =Data Availability Statement All observation data sets were provided by NASA GSFC’s CDAWeb at https://cdaweb.gsfc.nasa.gov while all ephemeris were obtained from SSCWeb at https://sscweb.gsfc.nasa.gov.

Authors=Sousasantos, J.; Rodrigues, F. S.; Gomez Socola, J.; Perez, C.; Colvero, F.; Martinis, C. R.; Wrasse, C. M.;Title=First Observations of Severe Scintillation Over Low-to-Mid Latitudes Driven by Quiet-Time Extreme Equatorial Plasma Bubbles: Conjugate Measurements Enabled by Citizen Science Initiatives, 2024, doi:10.1029/2024JA032545, ID:29097248. Keywords: space physics data facility, omniwebSample usage ( ACK ) =The authors acknowledge the NASA Space Physics Data Facility staff. Sample usage ( BODY ) =The geomagnetic indices Dst and Kp obtained at the NASA’s Space Physics Data Facility repository and the Auroral Electrojet (AE) index (quicklook version) from the World Data Center for Geomagnetism, Kyoto University, were used to assess the geomagnetic conditions under which the observations were made. Sample usage ( BODY ) =The Dst and Kp indices can be accessed at https://omniweb.gsfc.nasa.gov/form/dx1.html. AE index (Quicklook) is available at https://wdc.kugi.kyoto-u.ac.jp/ae_realtime/index.html .

Authors=Horvath, Ildiko; Lovell, Brian C.;Title=Investigating the Hot Zone Developed Under Short-Circuiting Conditions and the Coupled Magnetosphere-Ionosphere (M-I) System for the Subauroral Arc’s Inner-Magnetosphere Generation Environment, 2024, doi:10.1029/2024JA032552, ID:29097251.Keywords: cdaweb, omniSample usage ( ACK ) =We also gratefully acknowledge the 630 nm ASI images ( http://sirius.bu.edu/ ), the REGO ( https://data-portal.phys.ucalgary.ca/ ) images, the SSUSI auroral images ( https://ssusi.jhuapl.edu/gal_AUR ), and THEMIS ASI images, and the THEMIS and GOES data ( https://cdaweb.gsfc.nasa.gov/cdaweb/istp_public/ ). We gratefully acknowledge the World Data Center for Geomagnetism at Kyoto ( http://wdc.kugi.kyoto-u.ac.jp/wdc/Sec3.html ) and the OMNI database ( https://cdaweb.gsfc.nasa.gov/cdaweb/istp_public/ ) for providing the AE, AL and SYM-H indices. Sample usage ( BODY ) =The THEMIS and GOES data sets can be accessed online (through https://cdaweb.gsfc.nasa.gov/cdaweb/istp_public/ ). Sample usage ( ACK ) =We gratefully acknowledge the World Data Center for Geomagnetism at Kyoto ( http://wdc.kugi.kyoto-u.ac.jp/wdc/Sec3.html ) and the OMNI database ( https://cdaweb.gsfc.nasa.gov/cdaweb/istp_public/ ) for providing the AE, AL and SYM-H indices.

Authors=Zhou, Xuan; Gao, Xinliang; Lu, Quanming; Hajra, Rajkumar; Ke, Yangguang; Chen, Rui; Ma, Jiuqi;Title=Prompt Disappearance of Magnetospheric Chorus Waves Caused by High-Speed Magnetosheath Jets, 2024, doi:10.1029/2024JA032576, ID:29097252.Keywords: spdf, omniSample usage ( BODY ) =The OMNI data are obtained from the website http://spdf.gsfc.nasa.gov/pub/data/omni/. Sample usage ( BODY ) =Data Availability Statement The THEMIS data used in this study are obtained from the website http://themis.ssl.berkeley.edu/data/themis.

Authors=Gasparini, S.; Hatch, S. M.; Reistad, J. P.; Ohma, A.; Laundal, K. M.; Walker, S. J.; Madelaire, M.;Title=A Quantitative Analysis of the Uncertainties on Reconnection Electric Field Estimates Using Ionospheric Measurements, 2024, doi:10.1029/2024JA032599, ID:29097255.Keywords: spdf, omni, omniwebSample usage ( BODY ) =The OMNI data were obtained from the GSFC/SPDF OMNIWeb interface at https://omniweb.gsfc.nasa.gov/. The Lompe code and examples on how to run it and instructions on how to install it are available at https://github.com/klaundal/lompe. Sample usage ( BODY ) =Solar Wind and IMF Observations We use OMNI for solar wind and Interplanetary Magnetic Field (IMF) observations.

Authors=Rutala, M. J.; Jackman, C. M.; Owens, M. J.; Tao, C.; Fogg, A. R.; Murray, S. A.; Barnard, L.;Title=A Multi-Model Ensemble System for the Outer Heliosphere (MMESH): Solar Wind Conditions Near Jupiter, 2024, doi:10.1029/2024JA03261310.48550/arXiv.2402.19069, ID:29097256.Keywords: spdf, space physics data facility, omni, omni2, omni-2Sample usage ( BODY ) =A1 Table Boxcar-Smoothing Widths for Binarization, in Hours Source Epoch Ulysses (01) Ulysses (02) Ulysses (03) Juno in-situ 5 15 2 7 ENLIL 8 1 4 5 HUXt 1 9 1 1 Tao+ 6 11 2 10 Data Availability Statement Pre-processed spacecraft data were acquired from the Goddard Space Flight Center Space Physics Data Facility (SPDF) service (N. Papitashvili et al., 2015), except for the Juno in-situ data, which were instead acquired from Wilson et al. ( 2018) (plasma data) and via AMDA (Genot et al., 2021) (magnetic field data). Sample usage ( BODY ) =While no planet except for the Earth has a nearly continuous composite solar wind data set like OMNI, the outer planets are particularly data-poor in this regard owing to the rarity of distant-orbiting spacecraft missions and the short-lived nature of flyby missions. Sample usage ( BODY ) =The values here span the start of OMNI2 to the start of 2023 (27/11/1963-01/01/2023) and characterize the 10th-90th percentiles of all measurements.

Authors=Xiong, Senlin; Dai, Lei; Wang, Xu; Wang, Chi;Title=Rapid Relativistic Electron Enhancements During Van Allen Probes Era, 2024, doi:10.1029/2024JA032618, ID:29097257.Keywords: cdaweb, omni, omniwebSample usage ( BODY ) =Data Availability Statement The RBSP and GOES data are available at https://cdaweb.gsfc.nasa.gov/pub/data/. Geomagnetic index data is available at https://omniweb.gsfc.nasa.gov/. Sample usage ( BODY ) =Energetic electron flux data from the EPEAD and MAGED instruments aboard GOES 13, GOES 14, and GOES 15 satellites are utilized to quantify injections of seed (150 keV), subrelativistic (475 keV), and relativistic electrons (>800 keV) at GEO during REEs. The OMNI database provides AE/AL/AU and SYM-H indices. The SYM-H index is utilized to evaluate the phase and intensity of storms. Sample usage ( BODY ) =Geomagnetic index data is available at https://omniweb.gsfc.nasa.gov/.

Authors=Nilam, B.; Tulasi Ram, S.; Oliveira, Denny M.; Dimri, A. P.;Title=Role of Impact Angle on Equatorial Electrojet (EEJ) Response to Interplanetary (IP) Shocks, 2024, doi:10.1029/2024JA032638, ID:29097258.Keywords: cdawebSample usage ( ACK ) =Acknowledgments The authors acknowledge the open data policy of NASA/CDAWeb for solar wind particle and magnetic field data and SuperMAG for SMR index data. Sample usage ( BODY ) =The solar wind and magnetic field data are downloaded from the NASA/CDAWeb (Coordinated Data Analysis Web) interface ( https://cdaweb.gsfc.nasa.gov ).

Authors=Meenakshi, S.; Sridharan, S.;Title=Wavenumber-4 Longitudinal Structure in ICON-MIGHTI Thermospheric Meridional Wind, 2024, doi:10.1029/2024JA032642, ID:29097259.Keywords: spdfSample usage ( BODY ) =Data Availability Statement The ICON MIGHTI data products were retrieved from https://spdf.gsfc.nasa.gov/pub/data/icon/l2/.

Authors=Diaz Pena, Joaquin.; Zettergren, Matthew; Semeter, Joshua; Nishimura, Yukitoshi; Hirsch, Michael; Walsh, Brian M.;Title=3D Simulation of an Extreme SAID Flow Channel, 2024, doi:10.1029/2024JA032660, ID:29097260.Keywords: iriSample usage ( BODY ) =Various modeling techniques are available, ranging from empirical methods to complex physics-based numerical simulations. Empirical methods, such as IRI (Bilitza et al., 2022), NRLMSIS (Emmert et al., 2021), and NEQuick (Radicella, 2009), are based on mathematical functions derived from historical experimental data.

Authors=Svenningsson, I.; Yordanova, E.; Khotyaintsev, Yu. V.; Andre, M.; Cozzani, G.; Steinvall, K.;Title=Whistler Waves in the Quasi-Parallel and Quasi-Perpendicular Magnetosheath, 2024, doi:10.1029/2024JA03266110.48550/arXiv.2406.03060, ID:29097261.Keywords: omniSample usage ( BODY ) =Panel a shows the upstream magnetic field B SW from the OMNI database (Papitashvili King, 2020), measured by spacecraft positioned at the first Lagrangian point and propagated to the bow shock nose.

Authors=Qu, B. H.; Lu, J. Y.; Wang, Z. W.; Liu, J. J.; Wang, M.; Li, J. Y.; Zhang, H.;Title=Estimation of Ionospheric Field-Aligned Currents Using SuperDARN Radar and DMSP Observations, 2024, doi:10.1029/2024JA032708, ID:29097263.Keywords: international reference ionosphereSample usage ( BODY ) =The background atmospheres are based on the standard Naval Research Laboratory Mass Spectrometer Incoherent Scatter Radar (NRLMSISE-00) model (Picone et al., 2002) and the International Reference Ionosphere model (Bilitza Rawer, 1992). The GLOW model also incorporates a background ionization source, referred to as the background “nighttime” ionization.

Authors=Martinez, Benjamin C.; Lu, Xian; Pedatella, Nicholas M.; Wu, Haonan; Oberheide, Jens;Title=Impact of the Polar Vortex on Sub-Seasonal O/N2 Variability in the Lower Thermosphere Using GOLD and WACCM-X, 2024, doi:10.1029/2024JA032724, ID:29097264.Keywords: cdawebSample usage ( BODY ) =GOLD O/N 2 data can be found here: https://gold.cs.ucf.edu/data/search/ and here: https://cdaweb.gsfc.nasa.gov/pub/data/gold/ (long term archive). WACCM-X is part of the Community Earth System Model (CESM) and the source code is available at https://github.com/ESCOMP/CESM .

Authors=Aa, Ercha; Dzwill, Patricia; Zhang, Shun-Rong; Erickson, Philip J.;Title=A Statistical Analysis of the Morphology of Storm-Enhanced Density Plumes Over the North American Sector, 2024, doi:10.1029/2024JA032750, ID:29097266.Keywords: cdaweb, space physics data facilitySample usage ( BODY ) =The solar and geophysical parameters data is acquired from NASA’s Space Physics Data Facility/Coordinated Data Analysis Web service ( https://cdaweb.gsfc.nasa.gov/ ) and Kyoto world data center for Geomagnetism ( http://wdc.kugi.kyoto-u.ac.jp/ ).Sample usage ( BODY ) =The solar and geophysical parameters data is acquired from NASA’s Space Physics Data Facility/Coordinated Data Analysis Web service ( https://cdaweb.gsfc.nasa.gov/ ) and Kyoto world data center for Geomagnetism ( http://wdc.kugi.kyoto-u.ac.jp/ ).

Authors=Lu, Sheng; Xing, Zan-Yang; Zhang, Qing-He; Zhang, Yong-Liang; Yang, Hui-Gen; Oksavik, Kjellmar; Lyons, L. R.; Lockwood, Michael; Ma, Yu-Zhang; Wang, Xiang-Yu; Deng, Zhong-Xin; Xu, Tong; Li, Guo-Jun; Wang, Yong; Zhang, Duan;Title=A Statistical Study of Space Hurricanes in the Southern Hemisphere, 2024, doi:10.1029/2024JA032753, ID:29097267.Keywords: omni, omniwebSample usage ( BODY ) =Considering the solar wind response time from the bow shock nose to the dayside ionosphere, the OMNI data has been delayed by 7 min (Liou et al., 1998; Lockwood et al., 1989). Sample usage ( BODY ) =The solar wind, IMF, and geomagnetic indices were obtained from the NASA OMNI database ( https://omniweb.gsfc.nasa.gov/form/omni_min.html ). The event list of space hurricane in this study is available in Table S1.

Authors=Kato, Yuto; Shiokawa, Kazuo; Tanaka, Yoshimasa; Ozaki, Mitsunori; Kadokura, Akira; Oyama, Shin-ichiro; Oinats, Alexey; Connors, Martin; Baishev, Dmitry;Title=Spatiotemporal Development of Cosmic Noise Absorption at Subauroral Latitudes Using Multipoint Ground-Based Riometers, 2024, doi:10.1029/2023JA032206, ID:29535639.Keywords: cdaweb, space physics data facility, omni, omniwebSample usage ( ACK ) =We acknowledge use of National Aeronautics and Space Administration (NASA)/GSFC’s Space Physics Data Facility’s OMNIWeb (or Coordinated Data Analysis Web (CDAWeb) or ftp) service, and OMNI data (King Papitashvili, 2005; Papitashvili King, 2020). Sample usage ( BODY ) =The solar wind and IMF were provided by the NASA CDAWeb ( https://cdaweb.gsfc.nasa.gov/index.html ). The SYM-H index used in this paper was provided by the World Data Center-C2, Kyoto University and are available at https://wdc.kugi.kyoto-u.ac.jp/. The authors were also supported by the KAKENHI (Grant-in-Aid for Scientific Research; KS (JP 15H05815, JP 16H06286, 21H04518, 22K21345), SO: (21KK0059, 22H00173, 23K22554) from the Japan Society for the Promotion of Science. Sample usage ( BODY ) =IMF and solar wind parameters provided by OMNIWeb ( http://omniweb.gsfc.na-sa.gov/form/omni_min.html; King Papitashvili, 2005; Papitashvili King, 2020) were also used to investigate the relationship between CNA and interplanetary parameters.

Authors=Eyelade, A. V.; Stepanova, M.; Espinoza, C. M.; Antonova, E. E.; Kirpichev, I. P.;Title=The Response of the Earth Magnetosphere to Changes in the Solar Wind Dynamic Pressure: 1. Plasma and Magnetic Pressures, 2024, doi:10.1029/2023JA031948, ID:2953 5646.Keywords: spdf, space physics data facility, omni, omniwebSample usage ( BODY ) =The solar wind dynamic pressure and Interplanetary magnetic field (IMF) data were obtained from the OMNI database, through the Goddard Space Flight Center/Space Physics Data Facility (GSFC/SPDF) OMNIWeb interface at http://omniweb.gsfc.nasa.gov. Sample usage ( ACK ) =The authors gratefully acknowledge the OMNI database for the solar wind.Sample usage ( BODY ) =This is consistent with our argument and further justifies the use of 12-min averages of OMNI P SW values in our study, instead of longer times. The use of more than 10 years of THEMIS observations has enabled us to detect a number of features which, from our point of view, are very interesting. Sample usage ( ABSTRACT ) =We use 11-year Time History of Events and Macroscale Interactions during Substorms (THEMIS) instruments for plasma and magnetic field measurements in the magnetosphere and the OMNI database for solar wind dynamic pressure and IMF data. We focus on the effects of the solar wind dynamic pressure (PSW) and consider only times in which the interplanetary magnetic field (IMF) components are within +-5 nT.

Authors=Fleetham, A. L.; Milan, S. E.; Imber, S. M.; Bower, G. E.; Gjerloev, J.; Vines, S. K.;Title=The Relationship Between Large dB/dt and Field-Aligned Currents During Five Geomagnetic Storms, 2024, doi:10.1029/2024JA032483, ID:29535673.Keywords: omni, omniwebSample usage ( BODY ) =This included information such as the solar wind speed, density, IMF orientations and magnitudes, Auroral Upper and Lower indices and SYM-H values, accessed through the OMNI database (King Papitashvili, 2005). Observations The storm periods analyzed for this study were 28-29 May 2010, 8-11 March 2012, 23-26 April 2012, 17-20 March 2015 and 22-26 June 2015 (start and end dates included). Sample usage ( BODY ) =Finally, the 1-min resolution solar wind data used can be accessed from OMNIWeb via the link https://omniweb.gsfc.nasa.gov/form/omni_min.html.

Authors=Tan, Yusha; Lei, Jiuhou; Dang, Tong; Wang, Wenbin; Zhang, Binzheng; Luan, Xiaoli; Dou, Xiankang;Title=A Numerical Study of the High Latitudinal Ion-Neutral Coupling Time Scale Under Disturbed Conditions, 2024, doi:10.1029/2024JA032497, ID:29535684.Keywords: omniwebSample usage ( BODY ) =The solar wind and IMF data are available at NASA OMNIWeb ( https://omniweb.gsfc.nasa.gov/ ).

Authors=Yuan, H. C.; Li, L. Y.; Yang, L.; Cao, J. B.;Title=Competing Influences of Earthward Convection and Azimuthal Drift Loss on the Pitch Angle Distribution of Energetic Electrons, 2024, doi:10.1029/2024JA032534, ID:29535704.Keywords: cdaweb, omniSample usage ( BODY ) =Data Availability Statement The ACE data, GOES 13 data, GOES 15 data and SYM-H index are obtained from a the CDAWeb ( https://cdaweb.gsfc.nasa.gov/ ). The MagIES data can be retrieved from the Van Allen Probes Science Gateway at https://rbspgway.jhuapl.edu/ and the EMFISIS data are available at https://emfisis.physics.uiowa.edu/data/index. Sample usage ( ACK ) =We thank the Van Allen Probe MagEIS, EMFISIS and EFW groups for the data of energetic electrons, electric and magnetic fields, and also thank the ACE, GOES and OMNI groups for solar wind and geomagnetic indices. Sample usage ( BODY ) =Figure 2 displays the solar wind flow velocity ( V x ) from the OMNI database and the response of the inner magnetosphere at the Probe A location (including the dawn-dusk electric field ( E y ), the radial convection velocity ( V E x B = E y x B B 2 ${V}{E\times B}=\frac{{\boldsymbol{E}}{\boldsymbol{y}}\times \boldsymbol{B}}{{B}^{2}}$ ) and flux ( j ) of different-energy electrons).

Authors=Cantrall, C. E.; Mrak, S.; Paxton, L. J.; Zhang, Y.; Nikoukar, R.; Schaefer, R. K.; Yee, J. H.;Title=Source of the Observed Enhancements in Thermospheric SO/N2 During Two Solar Eclipses in 2023, 2024, doi:10.1029/2024JA032542, ID:29535718.Keywords: iriSample usage ( BODY ) =GLOW uses NRLMSIS-00 (Picone et al., 2002) and IRI-90 (Bilitza, 1990) to specify the neutral and ionosphere conditions, respectively.

Authors=Thomas, Dean; Weigel, Robert S.; Pulkkinen, Antti; Schuck, Peter W.; Welling, Daniel T.; Ngwira, Chigomezyo M.;Title=What Drove the Carrington Event? An Analysis of Currents and Geospace Regions, 2024, doi:10.1029/2024JA032556, ID:29535728.Keywords: spdf, sscwebSample usage ( BODY ) =This region includes both the plasma sheet (PS) and plasma sheet boundary layer (PSBL), and the +- 3 R E z ^ $\pm 3{R}_{E}\widehat{z}$ criteria is based on SPDF - Satellite Situation Center Web (SSCWeb) ( 2023) limits. Any remaining points from the SWMF grid are placed into the “other” region.

Authors=Chen, Rui; Gao, Xinliang; Yang, Zhongwei; Lu, Quanming; Kong, Zhenyu; Ma, Jiuqi; Ke, Yangguang; Wang, Chi;Title=Cross-Scale Energy Transfer From Ion-Scale to Electron-Scale Waves in the Earth’s Foreshock Region, 2024, doi:10.1029/2024JA032567, ID:29535730.Keywords: spdfSample usage ( BODY ) =Data Availability Statement The MMS data used in this study are available from the website https://spdf.gsfc.nasa.gov/pub/data/mms/ . The MMS data analysis is carried out using the publicly available Space Physics Environment Data Analysis System (SPEDAS, http://spedas.org ).

Authors=Fagundes, P. R.; Pillat, V. G.; Tardelli, A.; Muella, M. T. A. H.;Title=Pole-To-Pole Ionospheric Disturbances Due To Solar Flares, During Low Solar Activity, 2024, doi:10.1029/2024JA032597, ID:29535735.Keywords: omni, omniwebSample usage ( BODY ) =Also, SF X-ray and Dst data by: http://wdc.kugi.kyoto-u.ac.jp/ , http://omniweb.gsfc.nasa.gov/form/omni_min.html, http://acdb-ext.gsfc.nasa.gov/Data_services/met/ann_data.html, and INTERMAGNET for promoting high standards of magnetic observatory practice https://imag-data.bgs.ac.uk/GIN_V1/GINForms2 and EMBRACE http://www2.inpe.br/climaespacial/portal/en/.

Authors=Trigg, H.; Dorrian, G.; Boyde, B.; Wood, A.; Fallows, R. A.; Mevius, M.;Title=Observations of High Definition Symmetric Quasi-Periodic Scintillations in the Mid-Latitude Ionosphere With LOFAR, 2024, doi:10.1029/2023JA03233610.48550/arXiv.2312.04387, ID:29535739.Keywords: iri, international reference ionosphereSample usage ( BODY ) =Consequently we use estimated E- and F-region altitudes from the 2016 International Reference Ionosphere model (IRI: Bilitza et al., 2017) for this area which yielded hmE and hmF2 altitudes of 110 and 250 km respectively.

Authors=Srinivas, P.; Spencer, E.;Title=Determination of Outer Radiation Belt MeV Electron Energization Rates and Delayed Response Times to Solar Wind Driving During Geomagnetic Storms, 2024, doi:10.1029/2023JA032115, ID:29535742.Keywords: cdaweb, spdf, space physics data facilitySample usage ( ACK ) =Acknowledgments We acknowledge Van Allen Probes REPT, ACE Magnetic Field 16-Second Level 2 Data, ACE/SWEPAM Solar Wind Experiment 64-Second Level 2 Data, GOES-15 EPS (Energetic Particle Sensor) MagED (Magnetospheric Electron Detector) 1-min electron fluxes 40-475 keV-NOAA NGDC and SWPC data obtained from https://cdaweb.gsfc.nasa.gov/cgi-bin/eval2.cgi (NASA Goddard Space Flight Center Space Physics Data Facility (SPDF) CDAWeb data sets). Sample usage ( BODY ) =These parameters are the solar wind velocity v sw , the IMF B x IMF ${B}{x}^{\mathit{IMF}}$ , B y IMF ${B}{y}^{\mathit{IMF}}$ , B z IMF ${B}_{z}^{\mathit{IMF}}$ , and the solar wind proton density n sw , measured in GSM coordinates are obtained from ACE Magnetic Field 16-Second Level 2 Data and ACE/SWEPAM Solar Wind Experiment 64-Second Level 2 Data instruments obtained from CDAWeb. The input parameters are time delayed to account for the propagation of the solar wind to the nose of the magnetosphere at 10 R E as given in Spencer et al. ( 2007). We greatly appreciate the SuperMAG collaborators ( https://supermag.jhuapl.edu//info/?c. ( BODY ) =Data Availability Statement All the data used in this research is publicly available at the NASA Space Physics Data Facility at (NASA, 2023). SML data is available from the SuperMAG website (SuperMAG, 2023).

Authors=Lyu, Xingzhi; Jordanova, Vania K.; Engel, Miles; Tu, Weichao; Ma, Qianli;Title=Quantifying the Role of EMIC Wave Scattering During the 27 February 2014 Storm by RAM-SCB Simulations, 2024, doi:10.1029/2024JA032606, ID:29535743.Keywords: omniSample usage ( BODY ) =Simulation Results Simulations of Omni-Directional Fluxes Figure 1 shows the observed and simulated omni-directional electron fluxes along the orbit of Van Allen Probe B from 12 UT on February 27 to 12 UT on 28 February 2014, accompanied by the SYM-H index at the bottom panel.

Authors=Ito, Y.; Hosokawa, K.; Ogawa, Y.; Miyoshi, Y.; Tsuchiya, F.; Fukizawa, M.; Kasaba, Y.; Kazama, Y.; Oyama, S.; Murase, K.; Nakamura, S.; Kasahara, Y.; Matsuda, S.; Kasahara, S.; Hori, T.; Yokota, S.; Keika, K.; Matsuoka, A.; Teramoto, M.; Shinohara, I.;Title=On the Factors Controlling the Relationship Between Type of Pulsating Aurora and Energy of Pulsating Auroral Electrons: Simultaneous Observations by Arase Satellite, Ground-Based All-Sky Imagers and EISCAT Radar, 2024, doi:10.1029/2024JA032617, ID:29535746.Keywords: omniSample usage ( BODY ) =Figure 4e shows the energy flux of omni-directional electrons observed by MEP-e on board Arase in a format of the so-called Energy flux - time ( E - t ) diagram.

Authors=Tsurutani, Bruce T.; Sen, Abhijit; Hajra, Rajkumar; Lakhina, Gurbax S.; Horne, Richard B.; Hada, Tohru;Title=Review of the August 1972 and March 1989 (Allen) Space Weather Events: Can We Learn Anything New From Them?, 2024, doi:10.1029/2024JA03262210.48550/arXiv.2409.00452, ID:29535749.Keywords: omni, omniwebSample usage ( BODY ) =Thus, when the Sun has a very active AR causing many intense solar flares and ejecting many fast CMEs, the prediction of magnetic storms associated with solar AR intervals becomes far more difficult. There was OMNI data for the 4 August 1972 ICME but the magnetic field cutoff was ~44.3 nT with a data gap. Sample usage ( BODY ) =Data Availability Statement The IMP-5 proton fluxes for the August 1972 event are obtained from NASA’s OMNI web ( https://omniweb.gsfc.nasa.gov/ ). The Pioneer 10 IMF data for the August 1972 event are collected from NASA’s COHO web ( https://omniweb.gsfc.nasa.gov/coho/ ).

Authors=Ganushkina, N. Y.; van de Kamp, M.; Hoppe, T.; Dubyagin, S.; Gedalin, M.; Dimmock, A.; Lalti, A.; Khotyaintsev, Y. V.; Graham, D. B.; Vink, J.; Russell, C. T.;Title=SHARP Shock Database, 2024, doi:10.1029/2024JA032625, ID:29535752.Keywords: omni, omniwebSample usage ( BODY ) =Relaxation to a quiet downstream state, if any, may be very slow. For MMS shocks, OMNI data is used for the upstream parameters, and a complex elaborated procedure is applied for finding medians of the distributed values. Sample usage ( BODY ) =For the main shock parameters (Alfvenic Mach number M A, fast mode Mach number M f, the angle between the upstream magnetic field and the shock normal th Bn , and the upstream plasma beta b us ), the time-shifted OMNI database data from spacecraft located upstream of MMS ( https://omniweb.gsfc.nasa.gov/ ). In addition, the following parameters are also included: the upstream velocity, density, ion temperature, magnetic field vector, magnetic field magnitude, and the solar wind dynamic pressure for each shock crossing.

Authors=van Hazendonk, C. M.; Baddeley, L.; Laundal, K. M.; Chau, J. L.;Title=Detection and Energy Dissipation of ULF Waves in the Polar Ionosphere: A Case Study Using the EISCAT Radar, 2024, doi:10.1029/2024JA032633, ID:29535755.Keywords: spdf, omniweb, iri, international reference ionosphereSample usage ( BODY ) =The DSCOVR data were obtained from the GSFC/SPDF OMNIWeb Plus Browser interface at https://omniweb.gsfc.nasa.gov/ftpbrowser/dscovr_merged.html. Sample usage ( BODY ) =To calculate the frictional heating using Equation 4, direct ISR measurements provide T i , while neutral temperatures come from the NRLMSISE-00 model, and the ion densities from the International Reference Ionosphere 2016 (IRI-2016) model (Bilitza, 2018). The frictional heating is determined between 100 and 400 km.

Authors=Upadhyay, Kshitiz; Pallamraju, Duggirala; Chakrabarti, Supriya;Title=Estimation of Downward Heat Flux Into the F-Region From the Inner-Magnetosphere During Stable Auroral Red (SAR) Arc Events in the Daytime Obtained Using OI 630.0 nm Red-Line Emissions, 2024, doi:10.1029/2024JA032694, ID:29535776.Keywords: spdf, omniweb, iri, international reference ionosphere, vitmoSample usage ( BODY ) =Geomagnetic Indices To describe the geophysical conditions, daily averaged solar flux (F10.7) values measured in solar flux unit (sfu; 1sfu = 10 -22 Wm -2 Hz -1 ) and the hourly geomagnetic indices (Dst, Kp) attained from SPDF OMNIWeb were used. Geomagnetically quiet and disturbed periods were segregated with Kp 3 and Kp >= 3. Geomagnetic Coordinates were obtained for a given year using the OMNIWeb service at https://omniweb.gsfc.nasa.gov/vitmo/cgm.html. OI 630.0 nm Dayglow Observations The daytime ground-based observations of atomic oxygen 630.0 nm airglow were carried out using High-Resolution Imaging Spectrograph using Echelle grating (HIRISE, D. Sample usage ( BODY ) =In this work, the digisonde measured values of electron densities are fed instead of IRI electron densities to improve the accuracy of the GLOW model predicted emissions, while the positive ion densities are taken in proportion to maintain the charge-neutrality condition at each altitude. This apportionment is carried out as described in the IRI. The comparison of GLOW estimates with the HIRISE measured dayglow emissions will provide greater insights into the dynamics of ionosphere-thermosphere regions, especially during geomagnetic disturbances, as discussed in the next section. Sample usage ( BODY ) =For thermospheric neutral densities and temperatures, GLOW model uses Naval Research Laboratory Mass Spectrometer Incoherent Scatter (NRLMSIS-00) atmosphere (Picone et al., 2002) and International Reference Ionosphere (IRI-90) for ionospheric plasma (electron/ion) densities and their temperatures (Bilitza, 1990). Sample usage ( BODY ) =Geomagnetic Coordinates were obtained for a given year using the OMNIWeb service at https://omniweb.gsfc.nasa.gov/vitmo/cgm.html. OI 630.0 nm Dayglow Observations The daytime ground-based observations of atomic oxygen 630.0 nm airglow were carried out using High-Resolution Imaging Spectrograph using Echelle grating (HIRISE, D.

Authors=Bag, Tikemani; Ogawa, Y.; Sivakumar, V.;Title=Thermospheric NO Cooling During 2003 October “Halloween Storm”: Revisited, 2024, doi:10.1029/2024JA032805, ID:29535793.Keywords: omni, omniwebSample usage ( BODY ) =The modified 1-min resolution solar wind and interplanetary magnetic field data, shifted to Bow shock nose, are obtained from the OMNI web (https://omniweb.gsfc.nasa.gov/form/omni_min_def.html; King Papitashvili, 2005). Sample usage ( ACK ) =The authors thank the TIMED/SABER science team ( https://saber.gats-inc.com/ ), OMNIweb ( https://omniweb.gsfc.nasa.gov/ ), EISCAT (https://eiscat.se/) and CCMC (https://ccmc.gsfc.nasa.gov/) for providing the data used in this study. Sample usage ( BODY ) =The geomagnetic and IMF data are obtained respectively from the websites of OMNIWeb ( https://omniweb.gsfc.nasa.gov ). The Pederson conductivity and electric fields data are from EISCAT database ( https://eiscat.se/ ).

Authors=Li, L. Y.; Yang, L.; Cheng, K. X.; Cao, J. B.; Yang, J. Y.; Berthelier, J. J.;Title=Empirical Model of the Lowest Cutoff Altitude of Global Hiss Near Magnetic Equator, 2024, doi:10.1029/2024JA032886, ID:29535799.Keywords: cdaweb, omni, iriSample usage ( BODY ) =In addition, the geomagnetic AE index and the solar F10.7 radiation flux are obtained from the OMNI database in CDAWeb. Lowest Cutoff Altitude of Equatorial Hiss on Dayside and Nightside Figure 1 displays the power spectral densities ( E p , B p ) of electric and magnetic fields, wave polarization ellipticity and wave normal angle (WNA) during geomagnetically quiet times (AE 200 nT). Sample usage ( BODY ) =In addition, the geomagnetic AE index and the solar F10.7 radiation flux are obtained from the OMNI database in CDAWeb. Lowest Cutoff Altitude of Equatorial Hiss on Dayside and Nightside Figure 1 displays the power spectral densities ( E p , B p ) of electric and magnetic fields, wave polarization ellipticity and wave normal angle (WNA) during geomagnetically quiet times (AE 200 nT). Sample usage ( BODY ) =To examine whether the H + ions can maintain effective cyclotron motions at the lowest cutoff altitude of hiss waves, we compared the gyrofrequencies ( f e - ${f}{{\mathrm{e}}^{-}}$ , f H + ${f}{{\mathrm{H}}^{+}}$ , f O + ${f}{{\mathrm{O}}^{+}}$ ) of different plasma species (e - , H + , O + ) with the total collision frequency ( u ). f e - ${f}{{\mathrm{e}}^{-}}$ , f H + ${f}{{\mathrm{H}}^{+}}$ , and f O + ${f}{{\mathrm{O}}^{+}}$ are calculated with the magnetic field strength from the International Geomagnetic Reference Field model. u is a sum of the collision frequencies between different plasma species and between plasmas and neutral compositions, and it is calculated with the plasma parameters from the IRI model and the neutral parameters from the NRLMSIS 2.0 atmospheric model (Emmert et al., 2020).

Authors=Chisham, G.; Freeman, M. P.;Title=The Spatial Variation of Large- and Meso-Scale Plasma Flow Vorticity Statistics in the High-Latitude Ionosphere and Implications for Ionospheric Plasma Flow Models, 2024, doi:10.1029/2024JA032887, ID:29535801.Keywords: omniwebSample usage ( BODY ) =We use IMF data for the interval from OMNIWeb, which is lagged from the spacecraft to the Earth’s bow shock.

Authors=Lipatov, A. S.; Avanov, L. A.; Giles, B. L.; Gershman, D. J.;Title=Hybrid Kinetic Modeling of the Magnetosheath Impulsive Plasma Cloud Penetration Through the Magnetopause and Comparison With MMS and Other Spacecraft Observations, 2024, doi:10.1029/2024JA032909, ID:29535804.Keywords: cdawebSample usage ( BODY ) =Observation data from the WIND spacecraft were downloaded from CDAWeb ( https://cdaweb.gsfc.nasa.gov/cdaweb/istp_public/ ) and provided by A.

Authors=Xu, Xiang; Zhou, Chen; Wang, Zhuangkai; Du, Xiaohui;Title=Modeling the Propagation of Extremely Low Frequency Electromagnetic Emissions From the Power Lines to the Inner Magnetosphere in a Dipole Field, 2024, doi:10.1029/2023JA032403, ID:29535813.Keywords: iri, international reference ionosphereSample usage ( BODY ) =The NO + density is given as the sum of the densities of NO + and O 2 + ${\mathrm{O}}_{2}^{+}$ from IRI. Below 300 km, the O + density is given as the sum of the densities of O + and N + from IRI; above 350 km, the O + density is given by GCPM; from 300 to 350 km, the O + density profile is given by a smoothed average of both models in this region, similar to Pakhotin et al. ( 2022). Sample usage ( BODY ) =The plasma density in the ionosphere and the inner magnetosphere including electron, H + , He + , O + and NO + are obtained from the International Reference Ionosphere (IRI) model (e.g., Bilitza, 2001; Bilitza et al., 2022) and the Global Core Plasmasphere Model (GCPM) (e.g., Gallagher et al., 2000).

Authors=Michotte de Welle, B.; Aunai, N.; Lavraud, B.; Genot, V.; Nguyen, G.; Ghisalberti, A.; Smets, R.; Jeandet, A.;Title=Global Environmental Constraints on Magnetic Reconnection at the Magnetopause From In Situ Measurements, 2024, doi:10.1029/2023JA032098, ID:30743812. Keywords: cdaweb, space physics data facility, omniSample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s CDAWeb service, and OMNI data Computing resources used for the data analysis have been funded by the Plasapar federation. Sample usage ( BODY ) =It allows to access the data on the CDAweb database (https://cdaweb.gsfc.nasa.gov) for the THEMIS mission, and AMDA Budnik, 2011 for Cluster, DoubleStar, and MMS missions. Sample usage ( BODY ) =The solar wind velocity is taken from OMNI data as the average over a 5 min window centered around the measurement time to which is substracted the computed time shift.

Authors=Du, Wenyu; Zhong, Jiahao; Wan, Xin; Hao, Yongqiang; Xiong, Chao; Wang, Hui; Cui, Jun; Liu, Yiwen; Li, Qiaoling; Kuai, Jiawei;Title=Statistical Investigation of the Storm Time Plasma Density Strip-Like Bulges at Lower-Mid Latitudes, 2024, doi:10.1029/2024JA032608, ID:30743815.Keywords: spdf, omniwebSample usage ( BODY ) =GRACE KBR observation files are available at ( https://swarm-diss.eo.esa.int/#swarm%2FMultimission%2FGRACE%2FNE ).The solar wind and geomagnetic indices can be accessed in the GSFC/SPDF OMNIWeb database ( https://omniweb.gsfc.nasa.gov/ ). The CHAOS-7 model is provided by the Technical University of Denmark ( http://www.spacecenter.dk/files/magnetic-models/CHAOS-7/ ). The CHAOS-7 model is provided by the Technical University of Denmark ( http://www.spacecenter.dk/files/magnetic-models/CHAOS-7/ ).

Authors=Liao, J.; Kistler, L. M.; Mouikis, C. G.; Fuselier, S. A.; Hedlund, M.;Title=Assessing the Sources of the O+ in the Plasma Sheet, 2024, doi:10.1029/2024JA032635, ID:30743819.Keywords: omni, omniwebSample usage ( BODY ) =An example is shown in Figure 3, where panels (b) and (c) show the OMNI-directional energy spectra for H + and O +, and panels (e) and (f) show the parallel and anti-parallel spectra after subtraction of the bi-directional or isotropic contributions. Sample usage ( BODY ) =Dst and Kp Index and solar wind parameters are extracted from NASA/GSFC/s OMNI data set through OMNIWeb (King, Papitashvili, 2020; Matzka et al., 2021; Nose et al., 2015).

Authors=Mooney, M. K.; Forsyth, C.; Marsh, M. S.; Bradley, L.; Finnigan, T.; Forde, F.; Garrigan, F.; Mancini-Tuffier, C.; Mancini-Tuffier, T.; Roberts, E.; Vessoni, P.; Powell, J.; Clark, S.; Lao, C. J.; Smith, A.; Jackson, D. R.; Bingham, S.; Sharpe, M.; Hughes, T.; Chisham, G.; Milan, S.;Title=Evaluating Auroral Forecasts Against Satellite Observations Under Different Levels of Geomagnetic Activity, 2024, doi:10.1029/2023JA031478, ID:30743823.Keywords: cdawebSample usage ( BODY ) =IMAGE FUV data is archived at: https://cdaweb.gsfc.nasa.gov/pub/data/image/fuv/. Kp index data was provided by ISGI GFZ Potsdam.

Authors=Li, Li; Zhou, Xu-Zhi; Omura, Yoshiharu; Zong, Qiu-Gang; Liu, Ying; Rankin, Robert; Yue, Chao; Zhuang, Yan; Ren, Jie; Wang, Shan; Fu, Sui-Yan;Title=Nonlinear Drift-Bounce Resonance Between Charged Particles and Ultralow Frequency Waves, 2024, doi:10.1029/2024JA032742, ID:30743829.Keywords: spdfSample usage ( BODY ) =The Van Allen Probe data are available at the web https://spdf.gsfc.nasa.gov/pub/data/rbsp/.

Authors=Freund, Domenique; Blum, Lauren; Vidal-Luengo, Sergio; Bruno, Alessandro; Kataoka, Ryuho;Title=MeV Electron Precipitation During Radiation Belt Dropouts, 2024, doi:10.1029/2024JA032759, ID:30743834.Keywords: cdaweb, omni, omniwebSample usage ( BODY ) =Furthermore, NASA’s OMNIWeb data can be accessed online at https://cdaweb.gsfc.nasa.gov. Sample usage ( BODY ) =In addition to radiation belt electron data, solar wind data and geomagnetic indices (OMNI) are employed to enhance our comprehension of the background conditions during dropout and precipitation events. Sample usage ( BODY ) =Additionally, the combined pitch-angle resolved electron flux data from Van Allen Probes A and B are available via https://rbsp-ect.newmexicoconsortium.org/rbsp_ect.php, along with the corresponding Magnetic Ephemeris data ( https://rbsp-ect.newmexicoconsortium.org/science/DataDirectories.php ). Furthermore, NASA’s OMNIWeb data can be accessed online at https://cdaweb.gsfc.nasa.gov .

Authors=Chu, Xiangning; Bortnik, Jacob; Shen, Xiao-Chen; Ma, Qianli; Li, Wen; Ma, Donglai; Malaspina, David; Huang, Sheng; Hartley, David P.;Title=Imbalanced Regressive Neural Network Model for Whistler-Mode Hiss Waves: Spatial and Temporal Evolution, 2024, doi:10.1029/2024JA032761, ID:30743836. Keywords: omni, omniwebSample usage ( BODY ) =Additionally, solar wind parameters and geomagnetic indices, used as candidate inputs for the neural network model, are sourced from the OMNI data set (Papitashvili King, 2020) and SuperMAG (Gjerloev, 2012). Sample usage ( BODY ) =Solar wind parameters and geomagnetic indices are sourced from the OMNI data set (Papitashvili King, 2020) at omniweb.gsfc.nasa.gov, and from SuperMAG (Gjerloev, 2012) at https://supermag.jhuapl.edu/.

Authors=Zhu, Shengting; Luan, Xiaoli; Lei, Jiuhou;Title=Seasonal and Interhemispheric Variations of the Afternoon Auroral Responses to the Interplanetary Magnetic Field By Polarity, 2024, doi:10.1029/2024JA032417, ID:30743838.Keywords: omniwebSample usage ( BODY ) =The 1-min IMF data used here can be obtained from https://omniweb.gsfc.nasa.gov/.

Authors=Han, Yimin; Dai, Lei; Ren, Yong; Wang, Chi; Gonzalez, Walter; Zhu, Minghui;Title=Correlations of Plasma Properties Between the Upstream Magnetosheath and the Downstream Outflow Region of Magnetopause Reconnection, 2024, doi:10.1029/2024JA032817, ID:30743840.Keywords: cdaweb, omniSample usage ( BODY ) =ACE data is available at NASA CDA web ( https://cdaweb.sci.gsfc.nasa.gov/ ). SPEDAS routine used for data processing is available at http://spedas.org/blog/. Sample usage ( BODY ) =(b) V in GSM from MMS1. (c) Ion omni-directional differential energy fluxes from MMS1. (d-k) The magnetic field strength |B|, B in LMN coordinate system, Ion energy spectrum, ion density, V in LMN, ion bulk velocity |V|, Plasma b , and Alfven Mach number M A from MMS1 near the magnetopause reconnection region.

Authors=Cai, L.; Aikio, A.; Oyama, S.; Ivchenko, N.; Vanhamaki, H.; Virtanen, I.; Buchert, S.; Mekuriaw, M. L.; Zhang, Y.;Title=Effect of Polar Cap Patches on the High-Latitude Upper Thermospheric Winds, 2024, doi:10.1029/2024JA032819, ID:30743841.Keywords: spdf, omni, omniweb, iri, international reference ionosphereSample usage ( BODY ) =The OMNI data were obtained from the GSFC/SPDF OMNIWeb interface at https://omniweb.gsfc.nasa.gov ( https://doi.org/10.48322/45bb-8792 ). Sample usage ( ACK ) =Work of SO was supported by the joint research program of PPARC, Tohoku University. We acknowledge EISCAT, OMNI database, FMI IMAGE Magnetometer network, SuperMAG collaborators (Gjerloev, 2012), SuperDARN, and JHUAPL for providing the data (see also Open research section). Sample usage ( BODY ) =In addition, the solar wind and interplanetary magnetic field (IMF) conditions are analyzed using the 1-min data from the OMNI data set (Papitashvili King, 2020). The geomagnetic activity conditions are surveyed using several geomagnetic activity index products, including the local auroral electrojet indices (IE, IL, and IU) from the IMAGE network, SuperMAG auroral electrojet indices (SME, SML, and SMU), and Dst and Kp indices obtained from WDC in Kyoto, Japan. Sample usage ( BODY ) =The OMNI data were obtained from the GSFC/SPDF OMNIWeb interface at https://omniweb.gsfc.nasa.gov ( https://doi.org/10.48322/45bb-8792 ). Sample usage ( BODY ) =The ion compositions are taken from the International Reference Ionosphere 2016 (IRI-2016) model (Bilitza et al., 2017), and the neutral densities and temperatures are taken from the NRLMSISE-00 model (Peymirat et al., 2002).

Authors=Ashna, V. M.; Bhaskar, Ankush; Manju, G.; Sini, R.;Title=Solar Wind-Magnetosphere Coupling Efficiency and Its Dependence on Solar Activity During Geomagnetic Storms of 23-24 Solar Cycles, 2024, doi:10.1029/2023JA031687, ID:30743844.Keywords: cdaweb, spdf, space physics data facility, omniSample usage (BODY) =Data and Method of Analysis Data For the present work, the solar wind/interplanetary data of high time resolution (1 min time resolution) were obtained from the Space Physics Data Facility (SPDF) of NASA’s Goddard Space Flight Center (GSFC) (https://cdaweb.gsfc.nasa.gov/). We have used the OMNI (Combined 1AU IP Data; Magnetic and Solar Indices) database to study interplanetary and geomagnetic conditions during the identified events. Sample usage (BODY) =Data and Method of Analysis Data For the present work, the solar wind/interplanetary data of high time resolution (1 min time resolution) were obtained from the Space Physics Data Facility (SPDF) of NASA’s Goddard Space Flight Center (GSFC) (https://cdaweb.gsfc.nasa.gov/). Sample usage ( BODY ) =There is finite time required for the solar wind to travel from the spacecraft near the L1 point to the Earth. The OMNI interplanetary data accounts for this propagation delay. The OMNI data set shows the interplanetary data time-shifted to the Earth’s bow shock nose.

Authors=Jia, Yuanlin; Chen, Gang; Yan, Chunxiao; Xu, Jiyao; Zhang, Shaodong; Gong, Wanlin; Li, Yaxian; Hu, Pengfei;Title=Stripe-Like Echoes Scattered From Nighttime F-Region Field-Aligned Irregularities at Low-Latitudes, 2024, doi:10.1029/2024JA032868, ID:30743845.Keywords: omniwebSample usage ( BODY ) =These geomagnetic indexes can be freely accessed in the OMNIWeb ( 1963). Among them, Kp, SYM/H and IMF Bz indices are used to characterize the intensity of geomagnetic storm, AE can effectively represent the intensity of substorm, and PC index can be used to indicate the degree of the Joule heating produced by substorms.

Authors=Zhou, Su; Luan, Xiaoli; Zhou, Zhijin; Wu, Zongxian;Title=Nightside Detached Auroras Associated With Expanding Auroral Oval During the Main and Recovery Phases of a Magnetic Storm, 2024, doi:10.1029/2024JA032906, ID:30743847.Keywords: omni, omniwebSample usage ( BODY ) =The solar wind and geomagnetic activity indices are provided by the OMNI database. The solar wind data with time resolution of 1 min have been shifted to the bow shock of the Earth. Sample usage ( BODY ) =The OMNI data are available at https://omniweb.gsfc.nasa.gov/. The CARISMA geomagnetic pulsation data were obtained at http://data.carisma.ca/ICM/20Hz/.

Authors=Nishimura, Y.; Lyons, L. R.; Deng, Y.; Sheng, C.; Bristow, W. A.; Donovan, E. F.; Angelopoulos, V.; Nishitani, N.;Title=Obtaining Continental-Scale, High-Resolution 2-D Ionospheric Flows and Application to Meso-Scale Flow Science, 2024, doi:10.1029/2024JA032924, ID:30743849.Keywords: omniSample usage ( BODY ) =The SHF convection in the polar cap was enhanced after 06:20 UT, and it coincided with the IMF southward turning in the OMNI data (not shown). Because the background convection in SHF is parameterized by the IMF, the timing error in OMNI has a measurable impact on the convection map.

Authors=Zhou, Su; Luan, Xiaoli; Hou, Ying;Title=Multiple Satellite Observations of the High-Latitude Cusp Aurora During Northward IMF Conditions, 2024, doi:10.1029/2024JA032963, ID:30743851.Keywords: spdf, omni, omniwebSample usage (BODY) =The solar wind plasma parameters and geomagnetic indices, with time resolution of 1 min, are provided by the OMNI database (https://spdf.gsfc.nasa.gov/pub/data/omni). The solar wind and IMF parameters have been time-shifted to the location of the bow shock. Sample usage (BODY) =The OMNI data are available at https://omniweb.gsfc.nasa.gov/.

Authors=Yu, Jiang; Wang, Jing; Chen, Zuzheng; Ren, Aojun; Liu, Xiaoman; Liu, Nigang; Li, Liuyuan; Cui, Jun; Cao, Jinbin;Title=Statistical Distribution of the Peak Frequency of ECH Waves in the Outer Magnetosphere From Magnetospheric Multiscale Satellite Observations, 2024, doi:10.1029/2024JA032995, ID:30743853. Keywords: spdf, omniwebSample usage ( BODY ) =Data Availability Statement MMS data are available at the website https://spdf.gsfc.nasa.gov/pub/data/mms/. Solar wind data and geomagnetic indices are from OMNIWeb ( http://omniweb.gsfc.nasa.gov/ ).

Authors=Wu, Chen; Ridley, Aaron J.; Cullens, Chihoko Y.;Title=Seasonal Dependency of the Solar Cycle, QBO, and ENSO Effects on the Interannual Variability of the Wind DW1 in the MLT Region, 2024, doi:10.1029/2024JA032472, ID:30743858. Keywords: spdf, space physics data facility, omniwebSample usage ( BODY ) =The F10.7 index was provided by the NASA/GSFC’s Space Physics Data Facility’s OMNIWeb service ( https://spdf.gsfc.nasa.gov/ ).

Authors=Elhawary, R.; Laundal, K. M.; Reistad, J. P.; Madelaire, M.;Title=How Do Substorms Influence Hemispheric Asymmetries in Equivalent Currents?, 2024, doi:10.1029/2024JA032507, ID:30743861. Keywords: space physics data facility, omni, omniwebSample usage ( ACK ) =We acknowledge as well the use of NASA/GSFC’s Space Physics Data Facility’s OMNIWeb service, and OMNI data. Sample usage ( BODY ) =Solar wind measurements in GSM coordinates were acquired from the OMNI database. The GSM coordinate system is defined such that the x axis points toward the Sun, the y axis points duskward and is perpendicular to the Earth’s magnetic axis, and the z axis is the projection of the magnetic dipole axis onto the plane where the x axis is the normal vector. Sample usage ( ACK ) =We acknowledge as well the use of NASA/GSFC’s Space Physics Data Facility’s OMNIWeb service, and OMNI data.

Authors=Settino, A.; Nakamura, R.; Blasl, K. A.; Graham, D. B.; Nakamura, T. K. M.; Roberts, O. W.; Voros, Z.; Panov, E. V.; Simon Wedlund, C.; Schmid, D.; Hosner, M.; Volwerk, M.; Khotyaintsev, Yu. V.;Title=Plasma Mixing During Active Kelvin-Helmholtz Instability Under Different IMF Orientations, 2024, doi:10.1029/2024JA032513, ID:30743862. Keywords: omniSample usage ( BODY ) =The mixing parameter is a normalized quantity which ranges between [-1, 1] and is defined as follows: 1 m a = s a , a - s a , b s a , a + s a , b , ${\mu }{\alpha }=\frac{{\bar{\sigma }}{\alpha ,a}-{\bar{\sigma }}{\alpha ,b}}{{\bar{\sigma }}{\alpha ,a}+{\bar{\sigma }}_ {\alpha ,b}},$ 2 s a , a ( b ) = E a , a ( b ) f a ( E , t ) d E , ${\sigma }{\alpha ,a(b)}={\int }{{E}{\alpha ,a(b)}}{f}{\alpha }(E,t)\hspace*{.5em}dE,$ where s a , a ( b ) is the omni-directional particle distribution function, a = i , e is the index running on the particle species, a is the energy range corresponding to a MSH-like (low energy) particles, b is the energy range corresponding to MSP-like (high energy) particles, and finally the overline.

Authors=Picanco, G. A. S.; Denardini, C. M.; Nogueira, P. A. B.; Fagundes, P. R.; Meza, A. M.; Mendoza, L. P. O.; Padua, M. B.; Natali, M. P.; Resende, L. C. A.; Vital, L. F. R.; Title=On the Role of Physical Processes in Controlling Equatorial Plasma Bubble Morphology, 2024, doi:10.1029/2024JA03275610.22541/au.171395522.21458236/v1, ID:31168823.Keywords: omniwebSample usage ( ACK ) =Acknowledgments The authors would like to express their gratitude to the following networks and organizations for providing the GNSS data essential for this study: RBMC, RAMSAC, LISN, UNAVCO, NASA, BKG, IGM, and IGS. Special thanks to NASA/OMNIWeb for supplying the F10.7 data, and to IAGA/NOAA for providing the IGRF-13 model. Sample usage ( BODY ) =The F10.7 data is available on the NASA/OMNIWeb website ( https://omniweb.gsfc.nasa.gov/form/dx1.html ). The IGRF-13 Python version model can be found on the project page ( https://pypi.org/project/pyIGRF ).

Authors=Liu, Terry Z.; Angelopoulos, Vassilis; Otto, Antonius;Title=Observations of Compressional Structures Driven by Interaction Between Foreshock Ions and Discontinuities, 2024, doi:10.1029/2024JA032803, ID:31168829.Keywords: cdawebSample usage ( BODY ) =THEMIS data set are available at NASA’s Coordinated Data Analysis Web (CDAWeb, http://cdaweb.gsfc.nasa.gov/ ). The SPEDAS software (see Angelopoulos et al. (2019)) is available at http://themis.ssl.berkeley.edu.

Authors=Takahashi, Kazue; Lysak, Robert; Majmudar, Khilav;Title=Relationship Between Low-Latitude Pi2 Pulsations and Cavity Mode Oscillations, 2024, doi:10.1029/2024JA032858, ID:31168834.Keywords: space physics data facilitySample usage ( BODY ) =Data Availability Statement Van Allen Probes data are available at NASA Goddard Space Flight Center Space Physics Data Facility Coordinated Data Analysis Web ( 2024). Kakioka magnetometer data are available from Kakioka Magnetic Observatory ( 2013).

Authors=Liu, Xinlong; Zhang, Donghe; Coster, Anthea J.; Xu, Zhonghua; Shi, Xueling; Chakraborty, Shibaji;Title=The Morphology and Oscillations of Nightside Mid-Latitude Ionospheric Trough at Designated Longitudes in the Northern Hemisphere, 2024, doi:10.1029/2024JA032864, ID:31168835.Keywords: cdaweb, omniSample usage ( BODY ) =The SW and IMF data employed in this study were obtained from the OMNI data set hosted on the NASA Coordinated Data Analysis Web (CDAWeb). We utilized measurements including SW velocity, SW density, and the IMF B z ${B}_{z}$ component to investigate the association between the MLIT position oscillations and SW variations. Sample usage ( BODY ) =The SW and IMF data employed in this study were obtained from the OMNI data set hosted on the NASA Coordinated Data Analysis Web (CDAWeb).

Authors=Radhakrishnan, Dinesh K. V.; Fuselier, Stephen A.; Petrinec, Steven M.; Rice, Rachel C.; Nykyri, Katariina; Trattner, Karlheinz J.; Gershman, Daniel J.; Burch, James L.;Title=Evidence of Plasma Mixing at the Earth’s Magnetopause Due To Kelvin Helmholtz Vortices, 2024, doi:10.1029/2024JA032869, ID:31168836.Keywords: omniSample usage ( BODY ) =Choosing events in which IMF is constant allows us to reduce the impact of an important variable that controls the development of KHI at the magnetopause. In this study, IMF from OMNI data set is analyzed. KHI Properties Phase velocity, dominant period and wavelength are key parameters that define the characteristics of a KH wave (Zhou et al., 2022).

Authors=Alqeeq, S. W.; Fontaine, D.; Le Contel, O.; Akhavan Tafti, M.; Cazzola, E.; Atilaw, T.; Angelopoulos, V.; Auster, H. U.;Title=Global Compression of the Plasma Sheet and Magnetotail During Intense Storms From THEMIS Observations, 2024, doi:10.1029/2024JA032888, ID:31168837.Keywords: cdaweb, space physics data facility, omni, omniwebSample usage ( BODY ) =Data Availability Statement The data included in this study are publicly available at NASA/GSFC’s Space Physics Data Facility’s CDAWeb https://cdaweb.gsfc.nasa.gov/index.html/ , OMNIWeb services https://omniweb.gsfc.nasa.gov/ , and THEMIS data are available at the THEMIS data center https://themis.igpp.ucla.edu/overview_data.shtml . Sample usage ( BODY ) =Data Availability Statement The data included in this study are publicly available at NASA/GSFC’s Space Physics Data Facility’s CDAWeb https://cdaweb.gsfc.nasa.gov/index.html/ , OMNIWeb services https://omniweb.gsfc.nasa.gov/ , and THEMIS data are available at the THEMIS data center https://themis.igpp.ucla.edu/overview_data.shtml . Sample usage ( BODY ) =Data from the near-Earth heliospheric database OMNI (King Papitashvili, 2005) are displayed in Figure 1 with panel (b) representing the IMF magnitude and components, panel (c) the ion velocity components, panel (d) the dynamic pressure, panel (e) the particle density, panel (f) the plasma parameter beta and Alfvenic Mach number MA, where beta is the ratio between the thermal and magnetic pressures and MA the ratio of the solar wind and Alfvenic speeds. Sample usage ( BODY ) =Data Availability Statement The data included in this study are publicly available at NASA/GSFC’s Space Physics Data Facility’s CDAWeb https://cdaweb.gsfc.nasa.gov/index.html/ , OMNIWeb services https://omniweb.gsfc.nasa.gov/ , and THEMIS data are available at the THEMIS data center https://themis.igpp.ucla.edu/overview_data.shtml .

Authors=Kondrashov, D.; Drozdov, A. Y.; Shprits, Y.;Title=Nonlinear Wave-Particle Interaction Effects on Radiation Belt Electron Dynamics in 9 October 2012 Storm, 2024, doi:10.1029/2024JA032898, ID:31168838.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement Van Allen Probes MagEIS data is available at NASA Coordinated Data Analysis Web (CDAWeb) https://cdaweb.gsfc.nasa.gov/pub/data/rbsp/ . The NURD data set is available from ftp://rbm.epss.ucla.edu/ftpdisk1/NURD .

Authors=Fagundes, P. R.; Pillat, V. G.; Habarulema, J. B.; Tardelli, A.; Muella, M. T. A. H.;Title=Solar Flares and the Intricate Response of Earth’s Outer Geomagnetic Field Variation, 2024, doi:10.1029/2024JA032903, ID:31168839.Keywords: omni, omniwebSample usage ( BODY ) =Also, SF X-ray and Dst data by: http://wdc.kugi.kyoto-u.ac.jp/ , http://omniweb.gsfc.nasa.gov/form/omni_min.html , http://acdb-ext.gsfc.nasa.gov/Data_services/met/ann_data.html , and INTERMAGNET for promoting high standards of magnetic observatory practice https://imag-data.bgs.ac.uk/GIN_V1/GINForms2 and EMBRACE http://www2.inpe.br/climaespacial/portal/en/ .Sample usage ( BODY ) =Also, SF X-ray and Dst data by: http://wdc.kugi.kyoto-u.ac.jp/ , http://omniweb.gsfc.nasa.gov/form/omni_min.html , http://acdb-ext.gsfc.nasa.gov/Data_services/met/ann_data.html , and INTERMAGNET for promoting high standards of magnetic observatory practice https://imag-data.bgs.ac.uk/GIN_V1/GINForms2 and EMBRACE http://www2.inpe.br/climaespacial/portal/en/ .

Authors=Ellahouny, N. M.; Aikio, A. T.; Vanhamaki, H.; Virtanen, I. I.; Cai, L.; Marchaudon, A.; Blelly, P. -L.; Coster, A.; Norberg, J.; Maute, A.; Oyama, S. -I.;Title=EISCAT Observations of Depleted High-Latitude F-Region During an HSS/SIR-Driven Magnetic Storm, 2024, doi:10.1029/2024JA032910, ID:31168841.Keywords: cdaweb, space physics data facility, omni, omni-2, omniweb, iri, international reference ionosphereSample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s CDAWeb service and OMNI data for providing magnetic indices and solar wind parameters. Sample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s CDAWeb service and OMNI data for providing magnetic indices and solar wind parameters. Sample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s CDAWeb service and OMNI data for providing magnetic indices and solar wind parameters. We thank the institutes who maintain the IMAGE Magnetometer Array: Tromso Geophysical Observatory of UiT the Arctic University of Norway (Norway), Finnish Meteorological Institute (Finland), Institute of Geophysics Polish Academy of Sciences (Poland), GFZ German Research Centre for Geosciences (Germany), Geological Survey of Sweden (Sweden), Swedish Institute of Space Physics (Sweden), Sodankyla Geophysical Observatory of the University of Oulu (Finland), DTU Technical University of Denmark (Denmark), and Science Institute of the University of Iceland (Iceland). Sample usage ( BODY ) =Other Data Sources Solar wind 1-hr average data propagated to the Earth’s bow shock and magnetic indices (King Papitashvili, 2005) have been taken from the OMNI 2 database https://omniweb.gsfc.nasa.gov/html/ow_data.html , and those will be shown in Section 3.1. Sample usage ( BODY ) =Other Data Sources Solar wind 1-hr average data propagated to the Earth’s bow shock and magnetic indices (King Papitashvili, 2005) have been taken from the OMNI 2 database https://omniweb.gsfc.nasa.gov/html/ow_data.html , and those will be shown in Section 3.1. Sample usage ( BODY ) =The IRI model was used to calculate N e , I R I ${N}{e,IRI}$ and T i , I R I ${T}{i,IRI}$ values in a regular grid 1 deg ${}^{\circ}$ MLAT for each UT hour at a fixed longitude 106 deg ${}^{\circ}$ MLON corresponding to the radar scans. Sample usage ( BODY ) =Since the EISCAT data availability before the storm time is limited, we use the International Reference Ionosphere (IRI-2016) model (Bilitza, 2001; Bilitza et al., 2014, 2017) Fortran code to determine electron density N e $\left({N}{e}\right)$ and ion temperature T i $\left({T}{i}\right)$ background values for an altitude of 290 km.

Authors=Horvath, Ildiko; Lovell, Brian C.;Title=Investigating the 17 March 2013 Geomagnetic Storm Impacts on the Wholly Coupled Solar Wind-Magnetosphere-Ionosphere-Thermosphere System-Of-Systems, 2024, doi:10.1029/2024JA032917, ID:31168842.Keywords: cdaweb, omniSample usage ( BODY ) =The GOES data sets can be accessed online (through https://cdaweb.gsfc.nasa.gov/cdaweb/istp_public/ ). The Kp, AE, AL and SYM-H indices can be accessed online from the OMNI database (through https://cdaweb.gsfc.nasa.gov/cdaweb/istp_public/ ). Sample usage ( BODY ) =For monitoring solar and interplanetary conditions, we utilized various 1-min resolution ACE measurements and derived parameters provided by the OMNI database. Since the OMNI-provided ACE data sets are time shifted to the Earth bow shock nose, they can be compared to geomagnetic indices.

Authors=Guo, Deyu; Wang, Dedong; Shprits, Yuri; Xiang, Zheng; Ni, Binbin; Saikin, Anthony; Drozdov, Alexander Y.; Szabo-Roberts, Matyas; Wang, Jianhang; Liu, Yangxizi; Dong, Junhu;Title=One-Step Local Acceleration Process of Ultra-Relativistic Electrons in the Center of the Outer Radiation Belt: Observations, 2024, doi:10.1029/2024JA033024, ID:31168847.Keywords: spdf, omniSample usage ( BODY ) =Flux, density, and wave data of RBSP can be found at RBSP website ( https://spdf.gsfc.nasa.gov/pub/data/rbsp/ ). The PSD, m , K, and L* data we produced from the REPT instrument data with 5-min time resolution can be found at Guo ( 2024).Sample usage ( BODY ) =The first three panels show geomagnetic indexes (Kp in black and Dst in red) and solar wind parameters (dynamic pressure, solar wind speed in black and IMF Bz in red) with 1 h resolution from OMNI database. Figures 1d-1g shows the flux variations of 1.8, 3.4, 6.3 and 7.7 MeV electrons with 90deg local pitch angle observed by the Relativistic Electron Proton Telescope (REPT) instrument onboard RBSP twins (Baker et al., 2012).

Authors=Park, Jaeheung;Title=Total Magnetic Field Perturbations at Martian Low Altitudes (<=500 km): MAVEN Observations in 2014-2023, 2024, doi:10.1029/2024JA033029, ID:31168848.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement The MAVEN data used for this study are available at the NASA-CDAWeb ( https://cdaweb.gsfc.nasa.gov/pub/data/maven/insitu/kp-4sec/cdfs/ and https://cdaweb.gsfc.nasa.gov/pub/data/maven/mag/l2/sunstate-1sec/cdfs ).

Authors=Wang, C. Z.; Wang, H.; Zhang, K. D.; Zhong, Y. F.; Xia, H.; Sun, Y.; Cheng, Q. H.; Leng, Z. Y.;Title=Spatial Distribution and Wave Property of Dual-Frequency EMIC Waves: Swarm Observations, 2024, doi:10.1029/2024JA033031, ID:31168849.Keywords: space physics data facility, omniwebSample usage ( BODY ) =The solar wind and interplanetary magnetic field data as well as geomagnetic activity indices are available at NASA/GSFC’S Space Physics Data Facility’s OMNIWeb ( https://omniweb.gsfc.nasa.gov ). The availability of data from these websites to the public are appreciated.Sample usage ( BODY ) =The solar wind and interplanetary magnetic field data as well as geomagnetic activity indices are available at NASA/GSFC’S Space Physics Data Facility’s OMNIWeb ( https://omniweb.gsfc.nasa.gov ). The availability of data from these websites to the public are appreciated.

Authors=Zhai, Changzhi; Cai, Xuguang; Yu, Tingting; Peng, Wenjie; Cheng, Xiaoyun; Yue, Dongjie; Cai, Lei;Title=A Complete Chain of the Generating Processes of Ionospheric Negative Storm Over the North America, 2024, doi:10.1029/2024JA033091, ID:31168851.Keywords: omniwebSample usage ( BODY ) =Observational Data and the Numerical Model Geomagnetic Environment Indices The interplanetary magnetic field (IMF) north-south (Bz) and east-west (By) components in Geocentric Solar Magnetospheric (GSM) coordinates, symmetric ring current (SYMH), auroral electrojet (AE), Kp, and F10.7 indices during 3-6 November 2021 from the OMNIWeb database are used for this study. The HP index is based on the observed electron spectra by the Defense Meteorological Satellite Program (DMSP) satellite (Emery et al., 2009).

Authors=Guo, Xu; Zhao, Biqiang; Yu, Tingting; Hao, Honglian; Sun, Wenjie; Wang, Guojun; He, Maosheng; Mao, Tian; Li, Guozhu; Ren, Zhipeng;Title=East-West Difference in the Ionospheric Response During the Recovery Phase of May 2024 Super Geomagnetic Storm Over the East Asian, 2024, doi:10.1029/2024JA033170, ID:31168852.Keywords: space physics data facility, omni, omniwebSample usage ( BODY ) =Solar wind data were accessed through the NASA Goddard Space Flight Center’s Space Physics Data Facility ( https://omniweb.gsfc.nasa.gov/form/dx1.html ). The other data files used in this paper are available at Guo ( 2024).Sample usage ( BODY ) =The minutely interplanetary parameters are attained from the High Resolution OMNI (HRO) data set. The OMNI data set is an integrated collection of solar wind and geomagnetic field data, primarily used for space weather research. Sample usage ( BODY ) =Solar wind data were accessed through the NASA Goddard Space Flight Center’s Space Physics Data Facility ( https://omniweb.gsfc.nasa.gov/form/dx1.html ). The other data files used in this paper are available at Guo ( 2024).

Authors=Holmberg, M. K. G.; Jackman, C. M.; Taylor, M. G. G. T.; Witasse, O.; Wahlund, J. -E.; Barabash, S.; Michotte de Welle, B.; Huybrighs, H. L. F.; Imhof, C.; Cipriani, F.; Deprez, G.; Altobelli, N.;Title=Surface Charging of the Jupiter Icy Moons Explorer (JUICE) Spacecraft in the Solar Wind at 1 AU, 2024, doi:10.1029/2023JA032137, ID:31168854.Keywords: omniSample usage ( BODY ) =The values from the M1 data set have also been compared with the results from Venzmer and Bothmer ( 2018). They used hourly OMNI data from 1963 to 2016 to present the frequency distribution of proton temperature, and solar wind density, velocity, and magnetic field strength.

Authors=Lazzeri, Chiara; Samsonov, Andrey; Forsyth, Colin; Branduardi-Raymont, Graziella; Bogdanova, Yulia V.;Title=A Statistical Study of the Properties of, and Geomagnetic Responses to, Large, Rapid Southward Turnings of the Interplanetary Magnetic Field, 2024, doi:10.1029/2023JA032160, ID:31168855.Keywords: cdaweb, space physics data facility, omni, omniwebSample usage ( ACK ) =We gratefully acknowledge use of NASA/GSFC’s Space Physics Data Facility’s OMNIWeb (or CDAWeb or ftp) service, and OMNI data, and the SuperMAG collaborators ( https://supermag.jhuapl.edu/info/?Sample usage ( BODY ) =Data Availability Statement The OMNI data (solar wind IMF and plasma parameters, PCN and SYM-H) are available from the Coordinated Data Analysis Web ( http://cdaweb.gsfc.nasa.gov ), while SML and SMU data are available from the SuperMAG website ( https://supermag.jhuapl.edu/ ). Sample usage ( ACK ) =We gratefully acknowledge use of NASA/GSFC’s Space Physics Data Facility’s OMNIWeb (or CDAWeb or ftp) service, and OMNI data, and the SuperMAG collaborators ( https://supermag.jhuapl.edu/info/?Sample usage ( ACK ) =We gratefully acknowledge use of NASA/GSFC’s Space Physics Data Facility’s OMNIWeb (or CDAWeb or ftp) service, and OMNI data, and the SuperMAG collaborators ( https://supermag.jhuapl.edu/info/?Sample usage ( BODY ) =Finally, we examine whether the geomagnetic response to these “ST” events is different to more typical solar wind driving. OMNI Data The solar wind and magnetospheric data used in this study were obtained from the NASA/GSFC’s OMNI database ( https://omniweb.gsfc.nasa.gov/ ) (King Papitashvili, 2020). The OMNI solar wind and IMF data are 5-min resolution data measured by Wind, ACE, Geotail or IMP-8. Sample usage ( ACK ) =We gratefully acknowledge use of NASA/GSFC’s Space Physics Data Facility’s OMNIWeb (or CDAWeb or ftp) service, and OMNI data, and the SuperMAG collaborators ( https://supermag.jhuapl.edu/info/?Sample usage ( BODY ) =OMNI Data The solar wind and magnetospheric data used in this study were obtained from the NASA/GSFC’s OMNI database ( https://omniweb.gsfc.nasa.gov/ ) (King Papitashvili, 2020). The OMNI solar wind and IMF data are 5-min resolution data measured by Wind, ACE, Geotail or IMP-8.

Authors=Zhang, Yizhe; Varney, Roger H.;Title=A Statistical Survey of E-Region Anomalous Electron Heating Using Poker Flat Incoherent Scatter Radar Observations, 2024, doi:10.1029/2023JA032360, ID:31168858.Keywords: omniSample usage ( BODY ) =Panel (a) compares the yearly AEH occurrence frequency (events per day) to the smoothed F10.7 index from OMNI. Panel (b) is a scatter plot of AEH occurrences per 10 days versus the average AE index over 10 days.

Authors=Rout, Diptiranjan; Thampi, Smitha V.; Miyoshi, Yoshizumi; Pant, Tarun Kumar; Bhardwaj, Anil;Title=The Response of the Venusian Upper Atmosphere During the Passage of Interplanetary Coronal Mass Ejections, 2024, doi:10.1029/2024JA032553, ID:31168867.Keywords: omniSample usage ( BODY ) =As VEX entered the magnetosheath just after the bow shock at 08:21 UT, the spacecraft reaches the outer boundary of the magnetic barrier, where the external P dyn ${P}_{\mathit{dyn}}$ is equal to the total ionospheric pressure. 3 Figure From top to bottom, the panels show, for the event of 28 October 2013, variations of VEX observations in the Venus-Solar-orbital (VSO) coordinate system as a function of time in UT of the following parameters: Altitude of VEX (in km), each component of the magnetic field (Bx, By and Bz in nT), the magnitude of the magnetic field strength ( | B | $\vert B\vert $ in nT), the omni-directional energy spectrum of electron (E in eV), mean electron counts, the omni-directional energy spectra of proton (E in eV), O + ${O}^{+}$ ion (E in eV) and heavy-ion density c m - 3 $\left(\mathrm{c}{\mathrm{m}}^{-3}\right)$ during 08:30-10:30 UT.

Authors=Wang, Chih-Ping; Mouikis, C. G.; Wang, Xueyi; Masson, Arnaud; Lin, Yu;Title=Suprathermal Outflowing H+ Ions in the Lobe Driven by an Interplanetary Shock: 1. An Observation Event, 2024, doi:10.1029/2024JA032557, ID:31168868.Keywords: cdaweb, omniSample usage ( ACK ) =Papatashvilli at AdnetSystems, NASA Goddard Space Flight Center and CDAWeb for providing an open access to the OMNI data for free. We acknowledge Word Data Center for Geomagnetism, Kyoto for providing an open access to the SYM-H index for free.Sample usage ( BODY ) =The solar wind and IMF parameters and PC(N) index are available on NASA CDAWeb ( http://cdaweb.gsfc.nasa.gov/cdaweb/istp_public/ ). The SYM-H index from Word Data Center for Geomagnetism, Kyoto and the PC(N) index from National Space Institute (DTU Space), Technical University of Denmark are available on NASA CDAWeb ( http://cdaweb.gsfc.nasa.gov/cdaweb/istp_public/ ).Sample usage ( ACK ) =Papatashvilli at AdnetSystems, NASA Goddard Space Flight Center and CDAWeb for providing an open access to the OMNI data for free. We acknowledge Word Data Center for Geomagnetism, Kyoto for providing an open access to the SYM-H index for free.Sample usage ( BODY ) =The 1-min solar wind and IMF data and the SYM-H index are from OMNI. Note that the OMNI solar wind and IMF data have been propagated from the spacecraft locations in the upstream solar wind to the bow shock nose (Papitashvili King, 2020).

Authors=Day, E. K.; Grocott, A.; Walach, M. -T.; Wild, J. A.; Lu, G.; Ruohoniemi, J. M.; Coster, A. J.;Title=Observation of Quiet-Time Mid-Latitude Joule Heating and Comparisons With the TIEGCM Simulation, 2024, doi:10.1029/2024JA032578, ID:31168870.Keywords: cdaweb, spdfSample usage ( BODY ) =All solar wind data and geomagnetic indices were downloaded from NASA’s SPDF Coordinated Data Analysis Web ( https://cdaweb.gsfc.nasa.gov/index.html/ ). The AE data are also available from the WDC for Geomagnetism, Kyoto ( http://wdc.kugi.kyoto-u.ac.jp/wdc/Sec3.html ) who prepared this index. Sample usage ( BODY ) =All solar wind data and geomagnetic indices were downloaded from NASA’s SPDF Coordinated Data Analysis Web ( https://cdaweb.gsfc.nasa.gov/index.html/ ).

Authors=Bishop, Tyler B.; Blum, Lauren W.;Title=Global Maps of Plasmaspheric Erosion and Refilling for Varying Geomagnetic Conditions, 2024, doi:10.1029/2024JA032587, ID:31168872.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement The density data supporting this work come from the EMFISIS L4 density data product from the Van Allen Probes, which can be found at https://cdaweb.gsfc.nasa.gov/ . The Kp and DST indices were be obtained from the World Data Center for Geomagnetism, Kyoto (World Data Center for Geomagnetism et al., 2015), which can be found at https://wdc.kugi.kyoto-u.ac.jp/dst_final/index.html .

Authors=Adewuyi, M.; Keesee, A.; Ferdousi, B.;Title=Merging Mesoscale Magnetotail Features and Ground B-Field Perturbation Network Connectivity During Substorm Activity, 2024, doi:10.1029/2024JA032598, ID:31168875.Keywords: cdawebSample usage ( BODY ) =A 10-min time cadence database of these temperature maps can be found on CDAWEB (A. M. Keesee et al., 2020), and the codes for projection and temperature analysis can be found in the UNH Scholar repository (A.

Authors=Zhu, Minghui; Dai, Lei; Wang, Chi; Gonzalez, Walter; Samsonov, Andrey; Guo, Xiaocheng; Ren, Yong; Tang, Binbin; Xu, Qiuyu;Title=The Influence of Ionospheric Conductance on Magnetospheric Convection During the Southward IMF, 2024, doi:10.1029/2024JA032607, ID:31168876.Keywords: omni, omniwebSample usage ( BODY ) =Input Parameters The input parameters for numerical simulations are 1-min OMNI data from Interplanetary measurements. For the event on 11 March 2016, the OMIN data are obtained from the Wind spacecraft and time-shifted to the Earth’s bow shock (~10 R E ). Sample usage ( BODY ) =The OMNI data is available at https://omniweb.gsfc.nasa.gov .

Authors=Chen, Jinyuan; Ren, Xiaodong; Liu, Hang; Le, Xuan; Yang, Pengxi; Zhu, Wei; Zhang, Xiaohong;Title=Contributions of Ionospheric Migrating Tides to Ionospheric Intra-Annual Variations, 2024, doi:10.1029/2024JA032682, ID:31168881.Keywords: omniwebSample usage ( ACK ) =Acknowledgments We would like to express our gratitude to the Center for Orbit Determination in Europe (CODE) for providing their data, and to NASA’s OMNIWeb for supplying the F10.7 solar radio flux and sunspot number data. Sample usage ( BODY ) =The F10.7 index and sunspot number data were obtained from NASA’s OMNIWeb, while the Earth-Sun distance data were calculated using the Astropy library, a widely used Python package for astronomy (Collaboration et al., 2018; Robitaille et al., 2013).

Authors=Singh, D.; Goncharenko, L. P.; Galkin, I. A.; Chamberlin, P. C.; Redondo, F.;Title=Local Empirical Modeling of NmF2 Using Ionosonde Observations and the FISM2 Solar EUV Model, 2024, doi:10.1029/2024JA032697, ID:31168884.Keywords: iri, international reference ionosphereSample usage ( BODY ) =The IRI NmF2 used in this study is based on the URSI foF2 model plus the foF2 storm model in IRI. Sample usage ( ABSTRACT ) =Performance metrics demonstrate that the model parametrized using FISM2 has better accuracy than a similarly parametrized model with F10.7, as well as than the IRI-2020 model. Skill score metrics indicate that the FISM2 based model outperforms F10.7 model at all solar activity levels. Sample usage ( BODY ) =A typical application of ionosphere data reduction is for resolving long-term trends (e.g., Zossi et al., 2023) and interannual variability of ionospheric parameters. International Reference Ionosphere (IRI) and NeQuick are the two most widely used empirical models of the ionosphere (Bilitza et al., 2022; Nava et al., 2008).

Authors=Ray, Sayak; Huba, J. D.; Kundu, Bhaskar; Jin, Shuanggen;Title=Influence of the October 14, 2023, Ring of Fire Annular Eclipse on the Ionosphere: A Comparison Between GNSS Observations and SAMI3 Model Prediction, 2024, doi:10.1029/2024JA032710, ID:31168886.Keywords: space physics data facility, omniwebSample usage ( BODY ) =The above data sets are archived at NASA/GSFC’s Space Physics Data Facility’s OmniWeb service ( https://omniweb.gsfc.nasa.gov/form/dx4.html ). Magnetic activity indices describe variations in the geomagnetic field triggered by sudden irregular current systems.

Authors=Mourenas, Didier; Artemyev, Anton V.; Zhang, Xiao-Jia; Angelopoulos, Vassilis;Title=Impact of EMIC Waves on Electron Flux Dropouts Measured by GPS Spacecraft: Insights From ELFIN, 2024, doi:10.1029/2024JA032984, ID:31599023.Keywords: omniSample usage ( BODY ) =The LANL* code is freely available (LANL* CODE, 2024). OMNI data of S y m - H $Sym-H$ , K p $Kp$ , IMF B z ${B}_{z}$ , and P d y n $Pdyn$ are available from the Kyoto World Data Center for Geomagnetism (WDC FOR GEOMAGNETISM, 2024).

Authors=Hajra, Rajkumar; Tsurutani, Bruce Tsatnam; Lu, Quanming; Horne, Richard B.; Lakhina, Gurbax Singh; Yang, Xu; Henri, Pierre; Du, Aimin; Gao, Xingliang; Wang, Rongsheng; Lu, San;Title=The April 2023 SYM-H = -233 nT Geomagnetic Storm: A Classical Event, 2024, doi:10.1029/2024JA03298610.48550/arXiv.2409.08118, ID:31599025.Keywords: omniwebSample usage ( BODY ) =The near-Earth solar wind/interplanetary conditions are studied using the solar wind plasma and IMF data (1-min resolution) obtained from NASA’s OMNIWeb database ( https://omniweb.gsfc.nasa.gov/ ). These are observations made by spacecraft located in the solar wind upstream of the Earth, the data of which are shifted in time to take into account the propagation time of the solar wind from the upstream spacecraft to the Earth’s bow shock nose.

Authors=Moges, Samson T.; Kozlovsky, Alexander; Sherstyukov, Ruslan O.; Ulich, Thomas;Title=Solar Activity Dependence of Traveling Ionospheric Disturbance Amplitudes Using a Rapid-Run Ionosonde in High Latitudes, 2024, doi:10.1029/2024JA033013, ID:31599028.Keywords: iri, international reference ionosphereSample usage ( BODY ) =Since deriving the real hmF2 directly from our ionograms is a challenging task (Ulich et al., 2003), we utilize the International Reference Ionosphere (IRI) model. Subsequently, A R ${A}_{R}$ is multiplied by the ratio of the neutral density at a given time to the average neutral density.

Authors=Bower, G. E.; Imber, S.; Milan, S. E.; Schillings, A.; Fleetham, A. L.; Gjerloev, J. W.;Title=Location of Geomagnetic Disturbances in Relation to the Field Aligned Current Boundary, 2024, doi:10.1029/2024JA033039, ID:31599031.Keywords: cdaweb, space physics data facility, omni, omniwebSample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s CDAWeb service (at http://cdaweb.gsfc.nasa.gov ) and OMNI data. For the ground magnetometer data we gratefully acknowledge: INTERMAGNET, Alan Thomson; CARISMA, PI Ian Mann; CANMOS, Geomagnetism Unit of the Geological Survey of Canada; The S-RAMP Database, PI K. Sample usage ( BODY ) =The high resolution (1-min) OMNI data used in this study were obtained from the NASA Goddard Space Flight Center (GSFC) Space Physics Data Facility OMNIWeb portal at https://omniweb.gsfc.nasa.gov/form/om_filt_min.html. For the ground magnetometer data we gratefully acknowledge: INTERMAGNET, Alan Thomson; CARISMA, PI Ian Mann; CANMOS, Geomagnetism Unit of the Geological Survey of Canada; The S-RAMP Database, PI K. Sample usage ( BODY ) =Any GMDs that occur during AMPERE data gaps (7,094 GMDs) are removed from Figure 8. 8 Figure Barplot of GMD at each MLT that are associated with co-located positive field-aligned current (FAC) (red), negative FAC (blue), and no FAC (black). Finally the OMNI solar wind data is investigated at the time of the GMDs. As the OMNI data use is at 1 min resolution (King Papitashvili, 2005) the value is taken from the minute closest to the time of the GMD.

Authors=Edberg, Niklas J. T.; Andrews, David J.; Boldu, J. Jordi; Dimmock, Andrew P.; Khotyaintsev, Yuri V.; Kim, Konstantin; Persson, Moa; Auster, Uli; Constantinescu, Dragos; Heyner, Daniel; Mieth, Johannes; Richter, Ingo; Curry, Shannon M.; Hadid, Lina Z.; Pisa, David; Sorriso-Valvo, Luca; Lester, Mark; Sanchez-Cano, Beatriz; Stergiopoulou, Katerina; Romanelli, Norberto; Fischer, David; Schmid, Daniel; Volwerk, Martin;Title=Extent of the Magnetotail of Venus From the Solar Orbiter, Parker Solar Probe and BepiColombo Flybys, 2024, doi:10.1029/2024JA03260310.48550/arXiv.2410.21856, ID:31599032.Keywords: cdawebSample usage ( BODY ) =Parker Solar Probe data are available on the Coordinated Data Analysis Web (CDAWeb) at NASA Goddard Space Flight Center ( https://cdaweb.gsfc.nasa.gov/ ) (Bale, 2024).

Authors=Gonzalez, Gilda; Wu, Yen-Jung; Gasque, L. Claire; Triplett, Colin C.; Harding, Brian J.; Immel, Thomas J.;Title=Effects of Storm-Time Winds on Ionospheric Pre-Midnight Equatorial Plasma Bubbles Over South America as Observed by ICON and GOLD, 2024, doi:10.1029/2024JA033111, ID:31599041.Keywords: cdaweb, spdf, space physics data facility, omniwebSample usage ( BODY ) =Data Availability Statement The ICON data is available at https://icon.ssl.berkeley.edu/Data and https://cdaweb.gsfc.nasa.gov/pub/data/icon/. GOLD data is stored in https://gold.cs.ucf.edu/data/. Sample usage ( ACK ) =GOLD data is courtesy of NASA/GOLD and the mission science team and is archived at the NASA SPDF. NASA’s Explorers Program supports ICON through contracts NNG12FA45C and NNG12FA42I.Sample usage ( BODY ) =The data is available from NASA’s Space Physics Data Facility (SPDF) https://spdf.gsfc.nasa.gov/pub/data/gold/. To identify plasma bubbles, we visually inspect the NMAX (electrons/cm 3 )images derived from GOLD’s night disk scan (NI1) measurements for depletions in electron density. Sample usage ( BODY ) =Ey and Kp index are available on OmniWeb. The data used to characterize the presence of EPBs are from both the nighttime 135.6-nm images obtained by the NASA GOLD mission and topside F-region O + densities measured by the ICON Ion Velocity Meter (IVM) instrument.

Authors=Artemyev, Anton; Nishimura, Yukitoshi; Angelopoulos, Vassilis; Zhang, Xiao-Jia; Bortnik, Jacob;Title=Rapid Transport of Energetic Electrons to Low L-Shells: The Key Role of Electric Fields, 2024, doi:10.1029/2024JA033136, ID:31599043.Keywords: cdaweb, spdf, omni, omniwebSample usage ( BODY ) =The THEMIS, DMSP and SuperDARN data are available at https://cdaweb.gsfc.nasa.gov/, http://cedar.openmadrigal.org/, https://superdarn.jhuapl.edu. Sample usage ( BODY ) =Sym-H, Pdyn, and AE indexes were downloaded from the GSFC/SPDF OMNIWeb interface at https://omniweb.gsfc.nasa.gov or from https://supermag.jhuapl.edu. Sample usage ( BODY ) =Data and Method This study focuses on a detailed analysis of long-term (days) storm-time events, occurring on 30 November-1 December 2021 and 3-4 September 2022. For each event, we use the OMNI data set to obtain the Sym-H geomagnetic index (King Papitashvili, 2005).

Authors=Kurien, Leenamol V.; Kanekal, Shrikanth G.; Di Matteo, Simone; Greeley, Ashley D.; Schiller, Quintin; Shumko, Mykhaylo; Viall, Nicholeen M.; Kepko, Emil Lawrence;Title=Outer Zone Relativistic Electron Response to Mesoscale Periodic Density Structures in the Solar Wind: Van Allen Probes Measurements, 2024, doi:10.1029/2024JA032614, ID:31599044.Keywords: cdaweb, spdf, space physics data facility, omni, omniwebSample usage ( ACK ) =Acknowledgments The authors gratefully acknowledge collaborators in the NASA and CDAWeb team that have made available the data sets used in this study. Sample usage ( BODY ) =PDS are characterized using solar wind density measurements from the Solar Wind Experiment instrument (SWE) (Ogilvie et al., 1995), while interplanetary measurements from the OMNIWeb database ( https://cdaweb.gsfc.nasa.gov/index.html/ ) are used to provide overall event context. The IP data used in this study are time shifted from the spacecraft position to the nominal bow shock nose (Vokhmyanin et al., 2019). Sample usage ( BODY ) =Data Availability Statement The solar Wind plasma data and OMNIWeb database are available through the OMNI data set at the Space Physics Data Facility’s (SPDF) Coordinated Data Analysis Website at https://cdaweb.gsfc.nasa.gov/istp_public/ (Ogilvie et al., 1995). Sample usage ( ACK ) =We acknowledge data from the WIND, OMNI website, GOES, RBSP. The work was supported under the National Aeronautics and Space Administration Heliophysics Internal Scientist Funding Model (ISFM) program. Sample usage ( BODY ) =In order to set the context for our study, we show in Figure 1 an overview of the solar wind conditions, geomagnetic SYM-H and relativistic electron intensities for the period 17 January 2013. 1 Figure In situ interplanetary data from OMNI database propagated to bow shock (Vokhmyanin et al., 2019) and geomagnetic SYM-H index for 17 January 2013.

Authors=Usanova, M. E.; Woodger, L. A.; Blum, L. W.; Ergun, R. E.; Girard, C.; Gallagher, D. L.; Millan, R. M.; Sample, J. G.; Johnson, A. T.; Mann, I. R.;Title=H+, He+, He++, O++, N+ EMIC Wave Occurrence and Its Dependence on Geomagnetic Conditions: Results From 7 Years of Van Allen Probes Observations, 2024, doi:10.1029/2024JA032627, ID:31599049.Keywords: cdaweb, sscwebSample usage ( ACK ) =Acknowledgments We wish to thank the Van Allen Probes EMFISIS instrument team for data. We acknowledge CDAWeb, SSCWeb, SuperMag and Kyoto observatory for the use of their resources. Sample usage ( ACK ) =Acknowledgments We wish to thank the Van Allen Probes EMFISIS instrument team for data. We acknowledge CDAWeb, SSCWeb, SuperMag and Kyoto observatory for the use of their resources. Sample usage ( BODY ) =Data Availability Statement All the data used in this study are publicly available and can be accessed at. https://emfisis.physics.uiowa.edu/data/index (Van Allen Probes EMFISIS), https://sscweb.gsfc.nasa.gov (CDF files with Van Allen Probes orbital parameters), https://supermag.jhuapl.edu/indices/ (SME), https://omniweb.gsfc.nasa.gov/form/omni_min_def.html (SYMH and solar wind dynamic pressure).

Authors=Bag, Tikemani; Sivakumar, V.; Ogawa, Y.;Title=Impact of Interplanetary Shock on Thermospheric Cooling Emission: A Case Study, 2024, doi:10.1029/2024JA033176, ID:31599052.Keywords: spdf, omniwebSample usage ( BODY ) =The Ap, Kp, AE, and SYM-H indices are from SPDF OMNIWeb database (via https://omniweb.gsfc.nasa.gov ). Results and Discussion The solar and interplanetary magnetic field (IMF) along with SYM-H index data during 26 January 2017 are shown in Figure 1. Sample usage ( ACK ) =The solar and IMF data are obtained from WIND spacecraft via https://wind.nasa.gov. The SYM-H index is from OMNIWeb ( https://omniweb.gsfc.nasa.gov/ ). The Field-Aligned-Current is obtained from AMPERE/Iridium satellite constellation ( https://ampere.jhuapl.edu/ ). Sample usage ( BODY ) =The Ap, Kp, AE, and SYM-H indices are from SPDF OMNIWeb database (via https://omniweb.gsfc.nasa.gov ). Results and Discussion The solar and interplanetary magnetic field (IMF) along with SYM-H index data during 26 January 2017 are shown in Figure 1.

Authors=Wang, Yang; Zhong, Jun; Lee, Lou-Chuang; He, Jiansen; Zhang, Hui; Rong, Zhaojin; Wei, Yong;Title=Formation of Standing Whistler Wave in Earth’s Magnetosheath, 2024, doi:10.1029/2024JA03335810.22541/essoar.171632569.96681851/v1, ID:31599054.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement The MMS data used in this study are available at MMS Science Data Cente: https://lasp.colorado.edu/mms/sdc/public/search/; The THEMIS data used in this study are available at NASA’s CDAWeb ( https://cdaweb.gsfc.nasa.gov/index.html ).

Authors=Tian, S.; Wygant, J. R.; Cattell, C. A.; Dombeck, J. P.; Bortnik, J.;Title=Observations of Significant Ion Energy Outflows Associated With Cusp Ion Outflows and the Role of Poynting Flux as an Energy Source, 2024, doi:10.1029/2024JA032644, ID:31599076.Keywords: cdaweb, omniSample usage ( BODY ) =Data Availability Statement The Polar and Fast data are publicly accessible at https://cdaweb.gsfc.nasa.gov/data/polar/ and https://cdaweb.gsfc.nasa.gov/data/fast/ and through the Science Data Tool, available at http://sprg.ssl.berkeley.edu/~sdt/SdtReleases.html. Sample usage ( BODY ) =Polar data are shown on the left and Fast data are on the right. Panels a and b show the H+ omni-directional energy spectrogram and pitch angle spectrogram respectively.

Authors=Hirahara, Masafumi; Ebihara, Yusuke; Kitamura, Naritoshi; Sakanoi, Takeshi; Asamura, Kazushi; Takada, Taku; Saito, Hirobumi;Title=Reimei Satellite Observations of Alfvenic Interaction Modulating Inverted-V Electrons and Filamentary Auroral Forms at the Poleward Edge of a Discrete Arc, 2024, doi:10.1029/2024JA032650, ID:31599077. Keywords: omni, omniwebSample usage ( BODY ) =This feature also indicates that each of the calculated footprints shown in Figures 1h and 1i deviates from the practical position expected from the consistency with the electron signatures, which should be leftward by several (~4-7) pixels from the calculated footprints plotted in Figures 1h and 1i. According to the OMNI database (Papitashvili King, 2020), the solar wind velocity was ~605 km/s, the solar wind density was ~2 cm -3, and the Z (southward) component (B z ) of the interplanetary magnetic field (IMF) was -1.5 nT during the interval of interest. Sample usage ( BODY ) =The OMNI database is available at https://omniweb.gsfc.nasa.gov .

Authors=Li, Shaoyang; Ren, Zhipeng; Yu, Tingting; Zhao, Biqiang; Liu, Libo; Li, Guozhu; Yue, Xinan; Wei, Yong; Hu, Lianhuan;Title=A Case Study of Thermospheric Exospheric Temperature Responses During the G-Condition at Mohe and Beijing Stations, 2024, doi:10.1029/2024JA032653, ID:31599079. Keywords: space physics data facilitySample usage ( BODY ) =The Interplanetary Magnetic Field (IMF) By and Bz in the GSM coordinate, indices of Dst, 3-hourly Kp and F 10.7 shown in Figure 1 were downloaded from the Space Physics Data Facility website ( https://stereo-ssc.nascom.nasa.gov/ ). 1 Figure Temporal variations of Interplanetary magnetic field (IMF), geomagnetic activity and solar activity from 22 to 26 April (DOY 112-116) 2023.

Authors=Pedersen, M. N.; Juusola, L.; Vanhamaki, H.; Aikio, A. T.; Viljanen, A.;Title=Rapid Geomagnetic Variations During High-Speed Stream, Sheath and Magnetic Cloud-Driven Geomagnetic Storms From 1996 to 2023, 2024, doi:10.1029/2024JA032656, ID:31599087.Keywords: space physics data facility, omni, omniwebSample usage ( ACK ) =For the geomagnetic indices, solar wind and interplanetary magnetic field data we gratefully thank NASA/GSFC’s Space Physics Data Facility’s OMNIWeb ( https://omniweb.gsfc.nasa.gov/ ). We thank the institutes who maintain the IMAGE Magnetometer Array: Tromso Geophysical Observatory of UiT the Arctic University of Norway (Norway), Finnish Meteorological Institute (Finland), Institute of Geophysics Polish Academy of Sciences (Poland), GFZ German Research Centre for Geosciences (Germany), Geological Survey of Sweden (Sweden), Swedish Institute of Space Physics (Sweden), Sodankyla Geophysical Observatory of the University of Oulu (Finland), Polar Geophysical Institute (Russia), DTU Technical University of Denmark (Denmark), and Science Institute of the University of Iceland (Iceland). Sample usage ( BODY ) =The second to fifth panels show the 5 min resolution solar wind parameters and interplanetary magnetic field in geocentric solar magnetospheric (GSM) coordinates from OMNI during the time of the storm, and the shading indicates the active solar wind driver at that time. Sample usage ( ACK ) =For the geomagnetic indices, solar wind and interplanetary magnetic field data we gratefully thank NASA/GSFC’s Space Physics Data Facility’s OMNIWeb ( https://omniweb.gsfc.nasa.gov/ ). Sample usage ( BODY ) =The solar wind and interplanetary field data from OMNIWeb can be downloaded from https://omniweb.gsfc.nasa.gov/form/omni_min_def.html.

Authors=Sreelakshmi, J.; Maute, Astrid; Richmond, Arthur D.; Vichare, Geeta; Harding, Brian J.; Alken, Patrick;Title=Effect of Vertical Shear in the Zonal Wind on Equatorial Electrojet Sidebands: An Observational Perspective Using Swarm and ICON Data, 2024, doi:10.1029/2024JA032678, ID:31599128.Keywords: spdf, omniSample usage ( BODY ) =The ICON/MIGHTI Level 2.2 product Cardinal Vector Winds (Version 4) (Harding et al., 2023) is accessible from the ICON website https://icon.ssl.berkeley.edu/Data and SPDF ( https://spdf.gsfc.nasa.gov/data_orbits.html ). The geomagnetic activity index Kp (Matzka et al., 2021) was provided by the GFZ German Research Centre for Geosciences ( https://www.gfz-potsdam.de/en/section/geomagnetism/data-products-services/geomagnetic-kp-index ).

Authors=Chakraborty, Sayak; Palit, Sourav; Deb, Semontee; Basak, Tamal;Title=Modeling of the Variability of D-Region Ionospheric Electron Density During Solar Cycle-24, 2024, doi:10.1029/2024JA032700, ID:31599172.Keywords: iri, international reference ionosphereSample usage ( BODY ) =We do a first-order validation of the outcomes with IRI-2020 modeled electron density N e , i r i $\left({N}_{e,iri}\right)$ values and conclude with possible explanations of the reported results. Sample usage ( ABSTRACT ) =As a next-order validation, we compare our modeled Ne profiles with their IRI-2020 counterpart (Ne,iri). Their overall trends are found to be in agreement. Sample usage ( ACK ) =Acknowledgments Authors thank NCEI-NOAA for solar X-ray and sunspot number data, Laboratory of Atmospheric and Space Physics (LASP), University of Colorado for EUV light-curve, and International Reference Ionosphere model for electron density data. Sayak Chakraborty acknowledges the support of DST-INSPIRE fellowship (IF200266), Department of Science and Technology, Govt. of India.Sample usage ( BODY ) =The effects of the 11-year cycle of solar activity on the earth’s ionosphere have been studied in terms of Total Electron Content (TEC) (derived from the Global Positioning System, GPS), the International Reference Ionosphere (IRI-2020) model and the Thermosphere-Ionosphere Electrodynamics General Circulation Model (TIE-GCM) during C24 (Rao et al., 2019).

Authors=Chand, Atishnal Elvin; Bowden, George; Brown, Melrose;Title=Investigation of Thermospheric Response to Geomagnetic Storms Using GITM-OVATION Prime and -FTA Model With Comparison to GOLD and SABER Observations, 2024, doi:10.1029/2023JA031820, ID:31599218.Keywords: omniwebSample usage ( BODY ) =The IMF and solar wind data were taken from the OMNIWeb database, the Kp index from GFZ Potsdam, and the AE index from the SuperMAG website.

Authors=Li, Xing; Ren, Zhipeng; Cao, Jinbin;Title=The Non-Migrating DE3 Tide Response to the MJO Phenomenon at the MLT Altitudes, 2024, doi:10.1029/2024JA032792, ID:31599224.Keywords: cdawebSample usage ( ACK ) =Acknowledgments The TIMED/SABER temperature observations were provided through the website https://cdaweb.gsfc.nasa.gov/pub/data/timed/saber. The RMM index (Real-Time Multivariate MJO Index) were download through the website: http://www.bom.gov.au/climate/mjo/graphics/rmm.74toRealtime.txt.

Authors=Pandey, Kuldeep; Kalafatoglu Eyiguler, E. Ceren; Gillies, Robert G.; Danskin, Donald W.; Billett, Daniel D.; Yau, Andrew W.; Hussey, Glenn C.;Title=Differential Delay of Ordinary and Extraordinary Modes of Transionospheric Radio Waves, 2024, doi:10.1029/2024JA032798, ID:31599229.Keywords: iri, international reference ionosphereSample usage ( BODY ) =The foF2 values were fixed with latitude (gray lines) or varied with latitude (red, blue and sky-blue lines). 7 Figure The observed mode delay (black lines with circles) and ray-trace modeled mode delay using the electron density profiles from IRI-2020 for the RRI experiments. The model allowed for both a horizontally stratified ionosphere (fixed-foF2) and ones which varied with latitude (IRI-foF2, IRI-foF 2 x 1.15 $2\times 1.15$ , and IRI-foF 2 x 1.30 $2\times 1.30$ ). Sample usage ( BODY ) =The input electron density profiles are generated using the International Reference Ionosphere, IRI-2020 model (Bilitza et al., 2022). The ray paths from the ground transmitter to the satellite, at 1 s cadence, are calculated for both modes of radio wave propagation.

Authors=Li, Zhao; Engel, Miles; Hudson, Mary; Kress, Brian; Patel, Maulik; Selesnick, Richard;Title=The Impact of the 8-10 March 2012 Geomagnetic Storm on Inner Zone Protons as Measured by Van Allen Probes, 2024, doi:10.1029/2024JA032800, ID:31599231.Keywords: omniwebSample usage ( BODY ) =The time interval of the MHD-test particle simulation is highlighted in red while the storm interval is highlighted in green. 2 Figure (Top 3 panels) Solar wind parameters, geomagnetic indices and magnetopause location calculated using the Shue et al. ( 1998) model from OMNIWeb for 7 - 11 $7-11$ March 2012. (bottom) SEP flux (#/cm2/s/sr) measured by the west-facing EPS instrument on GOES-13 (Grubb, 1975).

Authors=Milan, S. E.; Bower, G. E.; Fleetham, A. L.; Imber, S. M.; Schillings, A.; Opgenoorth, H.; Gjerloev, J.; Paxton, L. J.; Vines, S. K.; Hubert, B.; Hairston, M. R.;Title=Occurrence and Causes of Large dB/dt Events and AL Bays in the Pre-Midnight and Dawn Sectors, 2024, doi:10.1029/2024JA032811, ID:31599238.Keywords: cdaweb, space physics data facility, omni, omniwebSample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s CDAWeb service and OMNI data. For the purpose of open access, the author has applied a Creative Commons Attribution (CC BY) license to the Author Accepted Manuscript version arising from this submission. Sample usage ( BODY ) =The IMAGE WIC data were obtained from CDAWeb ( https://cdaweb.gsfc.nasa.gov ). The DMSP/SSUSI file type EDR-AUR data were obtained from http://ssusi.jhuapl.edu (data version 0106, software version 7.0.0, calibration period version E0018). Sample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s CDAWeb service and OMNI data. For the purpose of open access, the author has applied a Creative Commons Attribution (CC BY) license to the Author Accepted Manuscript version arising from this submission. Sample usage ( BODY ) =Data Availability Statement The high resolution (1-min) OMNI data used in this study were obtained from the NASA Goddard Space Flight Center (GSFC) Space Physics Data Facility OMNIWeb portal at https://omniweb.gsfc.nasa.gov/form/om_filt_min.html ). Sample usage ( BODY ) =Solar wind and geomagnetic index data were accessed from the NASA/OMNI data set (Papitashvili King, 2020). The latitude of the AMPERE FACs was determined by fitting a circle to the boundary between the region 1 and region 2 currents (Milan, 2019; Milan et al., 2015), of which the radius, L ${\Lambda }$ , was used as a proxy for the open or polar cap flux content of the magnetosphere, F P C ${F}_{PC}$.

Authors=Walton, S. D.; Lejosne, S.; Claudepierre, S. G.;Title=The Global Characteristics of Electrons Near the Inner Edge of the Inner Radiation Belt, 2024, doi:10.1029/2024JA032883, ID:31599276.Keywords: omni, omniwebSample usage ( BODY ) =Data Availability Statement RBSP-ECT data are publicly available at https://rbsp-ect.newmexicoconsortium.org/science/DataDirectories.php OMNIWeb data (geomagnetic activity) are publicly available at https://omniweb.gsfc.nasa.gov/form/omni_min.html.

Authors=Vandas, M.; Romashets, E.;Title=Magnetic Field in the Earth’s Magnetosheath: Models Versus Observations, 2024, doi:10.1029/2023JA032393, ID:31599281.Keywords: cdaweb, omni, omniwebSample usage ( BODY ) =Data MSH magnetic field measurements were taken from the World Data Center (WDC) at NASA GSFC ( http://cdaweb.gsfc.nasa.gov/cdaweb/ ). We used 1-min averages provided by WDC from Cluster (FGM instrument, PIs A. Sample usage ( BODY ) =For upstream interplanetary values, 1-min averages of OMNI data (Wind KP shifted to the BS nose) from WDC ( https://omniweb.gsfc.nasa.gov/ ) were used. Sample usage ( BODY ) =For upstream interplanetary values, 1-min averages of OMNI data (Wind KP shifted to the BS nose) from WDC ( https://omniweb.gsfc.nasa.gov/ ) were used. We have received hints for BS and MP crossings in lists by Kruparova et al. ( 2019) and Lalti et al. ( 2022); in addition, we used identified crossings from our previous analysis (Vandas et al., 2020).

Authors=Xiang, L.; Lee, K. H.; Lee, L. C.; Wu, D. J.; Chen, L.; Feng, H. Q.; Li, Q. H.; Zhao, G. Q.;Title=Proton Temperature Anisotropy Constraint Associated With Alpha Beam Instability in the Solar Wind, 2024, doi:10.1029/2023JA032398, ID:31599291.Keywords: spdfSample usage ( ACK ) =We are grateful to the Wind team for providing the data ( https://spdf.gsfc.nasa.gov/pub/data/wind/ ) and NCHC in Taiwan for providing computational and storage resources.

Authors=Sergeev, V. A.; Stepanov, N. A.; Ogawa, Y.; Rozanov, E. V.; Shukhtina, M. A.;Title=Local Time Distribution and Activity Dependence of Extreme Electron Densities in the Auroral D-Region as an Image of Energy-Dependent Energetic Electron Precipitation, 2024, doi:10.1029/2024JA032913, ID:31599309.Keywords: omni, omniwebSample usage ( BODY ) =Gjerloev for making the SuperMAG indices available at http://supermag.jhuapl.edu/. Data from OMNI data base are available from https://omniweb.gsfc.nasa.gov/index.html and AE index data are available from the World Data Center for Geomagnetism at Kyoto University at http://wdc.kugi.kyoto-u.ac.jp/.

Authors=Gann, Ayden L. S.; Yigit, Erdal;Title=Ionospheric and Thermospheric Effects of Hurricane Grace in 2021 Observed by Satellites, 2024, doi:10.1029/2024JA032933, ID:31599314.Keywords: space physics data facilitySample usage ( BODY ) =GOLD level 2 data (Eastes et al., 2020a, 2020b) Available via: GOLD Science Data Center and NASA’s Space Physics Data Facility URL: https://gold.cs.ucf.edu/search/. MERRA-2 data (GMAO, 2015) Available from: Global Modeling and Assimilation Office Access: Freely accessible with registration required URL: https://doi.org/10.5067/0TUFO90Q2PMS.

Authors=Du, Yingshuai; Liu, Wenlong; Zhang, Dianjun; Tan, Xin; Dunlop, Malcolm W.;Title=Latitudinal Distribution of Dayside Magnetospheric Currents Based on Cluster Observations, 2024, doi:10.1029/2024JA032943, ID:31599316.Keywords: omniSample usage ( BODY ) =Methodology and Data Processing Magnetic field data from the FGM instrument (Balogh et al., 2001), proton data from the Cluster Ion Spectrometer/Composition and Distribution Function (CIS/CODIF) instrument (Reme et al., 2001), solar wind flow speed, dynamic pressure, and Kp index from the OMNI database are used in this study. The curlometer method developed by Dunlop et al. ( 1988) and Dunlop ( 2002) is used in this study to calculate the current density.

Authors=Wang, Shan; Li, Jing-Huan; Li, Li; Zhou, Xu-Zhi; Omura, Yoshiharu; Zhao, Jiu-Tong; Liu, Zhi-Yang; Zong, Qiu-Gang; Zhang, Hui; Yue, Chao;Title=A Statistical Examination of Interactions Between 1-Hz Whistler Waves and Ions in the Earth’s Foreshock, 2024, doi:10.1029/2024JA032960, ID:31599338. Keywords: spdf, space physics data facility, omniSample usage ( BODY ) =OMNI data are from the Space Physics Data Facility (SPDF, 2024). The data analysis is conducted using the publicly available SPEDAS software (SPEDAS, 2024). Sample usage ( BODY ) =We have tested that in the solar wind, the electron density and bulk velocity well agree with the OMNI data set, confirming the reliability of electron measurements for solar wind populations.

Authors=Zhou, Yaxiong; Gao, Yang; Gao, Zhonglei; Liu, Si; Yang, Hongming; Shi, Chen; Yang, Qiwu; Tang, Jiawen; Wang, Bowen; Xiao, Fuliang;Title=Simultaneous Occurrence of Electromagnetic and Quasi-Electrostatic Magnetosonic Waves, 2024, doi:10.1029/2024JA032967, ID:31599339.Keywords: spdf, omniSample usage ( BODY ) =Data Availability Statement Data sets for this research are available at the following website: https://spdf.gsfc.nasa.gov/pub/data/rbsp/. Sample usage ( BODY ) =(a) Geomagnetic activity indices of AE and SYM-H; (b) magnetic field power spectral densities P B ${P}{\mathrm{B}}$ ; (c) electric field power spectral densities P E ${P}{\mathrm{E}}$ ; (d) omni-directional differential fluxes of protons j $j$ ; (e) background electron densities n e ${n}_{\mathrm{e}}$.

Authors=Liu, Yangxizi; Xiang, Zheng; Ni, Binbin; Zhou, Chen; Wang, Jianhang; Guo, Deyu; Dong, Junhu; Hu, Jingle; Guo, Haozhi;Title=Longitudinal Variations of Energetic Electrons Scattered by NWC Transmitter: DEMETER Observations, 2024, doi:10.1029/2024JA032975, ID:31599340.Keywords: omniwebSample usage ( BODY ) =The geomagnetic indexes are obtained through https://omniweb.gsfc.nasa.gov.

Authors=Saint-Girons, Emile; Zhang, Xiao-Jia; Mourenas, Didier; Artemyev, Anton V.; Angelopoulos, Vassilis;Title=Omnidirectional Energetic Electron Fluxes From 150 to 20,000 km: An ELFIN-Based Model, 2024, doi:10.1029/2024JA03297710.48550/arXiv.2406.05579, ID:31599342. Keywords: omniSample usage ( BODY ) =Shi et al., 2024; Wong et al., 2022). Then, the inferred J omni ( h , E ) ${J}{\mathit{omni}}(h,E)$ should remain within a factor of 2 ${\approx} 2$ from the actual J omni ( h , E ) ${J}{\mathit{omni}}(h,E)$ at h h max $h {h}_{\max }$.

Authors=Zhang, Kedeng; Wang, Hui; Song, Huimin;Title=The Polarity Oscillations of the Equatorial Electrojet in Response to the Geomagnetic Storm on 1 December 2023, 2024, doi:10.1029/2024JA032978, ID:31599343.Keywords: omni, omniwebSample usage ( BODY ) =Data Availability Statement The solar wind data is downloaded from OMNI ( https://omniweb.gsfc.nasa.gov/form/dx1.html ). Swarm observed EEJ can be downloaded at https://swarm-diss.eo.esa.int/#swarm/Level2daily/Latest_baselines.

Authors=Wu, Fang; Jiao, Jing; Du, Lifang; Zheng, Haoran; Wang, Zelong; Cheng, Xuewu; Wu, Fuju; Xia, Yuan; Wang, Jiqin; Wang, Wei; Wang, Kexin; Xun, Yuchang; Xu, Jiyao; Zhu, Yajun; Yuan, Wei; Liu, Weijun; Yang, Guotao;Title=A Three-Frequency Ca+ Doppler Lidar for Ion Temperature Measurements in the E and F Regions, 2024, doi:10.1029/2024JA032511, ID:31599356.Keywords: cdaweb, space physics data facility, iri, international reference ionosphereSample usage ( BODY ) =The temperature data of ICON are available for download from the ICON website hosted by the Berkeley Space Sciences Laboratory ( https://icon.ssl.berkeley.edu/Data ) and from the NASA Space Physics Data Facility https://cdaweb.gsfc.nasa.gov/pub/data/icon/. Sample usage ( BODY ) =The International Reference Ionosphere model (IRI-2016) is included for temperature comparison. The IRI-2016 model is an empirical model that provides primary ionospheric parameters such as neutral temperature, electron temperature and ion temperature (Bilitza et al., 2017, 2022). The IRI model’s major data sources include ISR. Its performance varies by region. Sample usage ( BODY ) =Figures 8e-8h show the four measurements of the ion temperatures.

Authors=Yu, Chao; Zhang, Xiao-Xin; Wang, Wenbin; He, Fei;Title=Hemispheric Asymmetry of Ionospheric Poynting Flux During Geomagnetically Quiet Periods, 2024, doi:10.1029/2024JA032519, ID:31599358.Keywords: omniwebSample usage ( BODY ) =The Kp index are publicly available from https://omniweb.gsfc.nasa.gov/form/dx1.html .

Authors=Haas, Bernhard; Shprits, Yuri Y.; Himmelsbach, Julia; Wang, Dedong; Drozdov, Alexander Y.; Szabo-Roberts, Matyas.; Hanzelka, Miroslav;Title=Modeling Pitch Angle Dependent Electron Precipitation Using Electron Lifetimes, 2024, doi:10.1029/2024JA032554, ID:31599398.Keywords: spdf, omniwebSample usage ( BODY ) =D1 Table Input Models for the VERB-4D Runs Input Model Electric field Volland-Stern (Maynard Chen, 1975; Stern, 1975; Volland, 1973) Magnetic field T89 (Tsyganenko, 1989) Initial condition Taken from satellite measurements (for details, see Haas et al., 2023) Radial diffusion coefficient Brautigam and Albert ( 2000) Chorus and Hiss diffusion coefficients Wang et al. ( 2020) Chorus electron lifetimes Wang et al. ( 2022) and Haas et al. ( 2023) Hiss electron lifetimes Orlova et al. ( 2016) Plasmapause location Carpenter and Anderson ( 1992) Upper radial boundary condition Denton et al. ( 2015) (extrapolated to energies above 40 keV by assuming an exponential continuation) Lower V $V$ boundary condition < f > V = 0 $\frac{\partial \langle f\rangle }{\partial V}=0$ Upper V $V$ boundary condition < f > = 0 $\langle f\rangle =0$ Lower K $K$ boundary condition < f > K = 0 $\frac{\partial \langle f\rangle }{\partial K}=0$ Upper K $K$ boundary condition < f > K = 0 $\frac{\partial \langle f\rangle }{\partial K}=0$ Data Availability Statement POES TED data is publicly available at the website https://spdf.gsfc.nasa.gov/pub/data/noaa/. Kp time histories are available at the NASA OMNIWeb data explorer, accessible at https://omniweb.gsfc.nasa.gov/form/dx1.html .Sample usage ( BODY ) =Kp time histories are available at the NASA OMNIWeb data explorer, accessible at https://omniweb.gsfc.nasa.gov/form/dx1.html.

Authors=Shahid, Muhammad; Bashir, M. Fraz; Artemyev, A. V.; Zhang, X. -J.; Angelopoulos, Vassilis; Murtaza, G.;Title=Statistical Properties of Quasi-Periodic Electromagnetic Ion Cyclotron Waves: ULF Modulation Effects, 2024, doi:10.1029/2023JA03229010.22541/essoar.170067176.69596243/v1, ID:32032741.Keywords: omniSample usage ( BODY ) =It is important to carefully check these uncertainties before applying this method to analyze density-based parameters in EMIC wave interactions with charged particles, as they are crucial for accurately interpreting the results. 1 Figure Three example events (22 June 2017 from THEMIS-A, 12 October 2017 and 14 September 2018 from THEMIS-E) with quasi-periodic EMIC waves: (a) magnetic field components in GSM coordinates, (b) f p e / f c e ${f}{pe}/{f}{ce}$ ratio using spacecraft potential (red) and ESA measurements (black), (c) ultra-low frequency d B $\delta {B}{{\Vert} }$ field, (d) omni-directional spectrum of ions, (e) pitch-angle distribution (f) EMIC wave magnetic field spectrum with overplotted white lines of cyclotron frequency of proton f c p $\left({f}{cp}\right)$ and Helium f cHe $\left({f}_{\mathit{cHe}}\right)$ , (g) EMIC wave ellipticity, (h) EMIC wave normal angle.

Authors=Wang, Hui; Cheng, Qihang; Luhr, Hermann; Zhong, Yunfang; Zhang, Kedeng; Xia, Hao;Title=Local Time and Hemispheric Asymmetries of Field-Aligned Currents and Polar Electrojet During May 2024 Superstorm Periods, 2024, doi:10.1029/2024JA033020, ID:32032742.Keywords: space physics data facility, omni, omniwebSample usage ( BODY ) =The solar wind and interplanetary magnetic field and magnetic activity index data are from NASA/GSFC’S Space Physics Data Facility’s OMNIWeb ( https://omniweb.gsfc.nasa.gov ).Sample usage ( BODY ) =For describing interplanetary conditions, 1-min IMF and solar wind velocity data time-shifted to the bow shock have been obtained from the OMNI website. Observation Results The event examined occurred on 09-13 May 2024 and was driven by CME observed in the solar wind. Sample usage ( BODY ) =The solar wind and interplanetary magnetic field and magnetic activity index data are from NASA/GSFC’S Space Physics Data Facility’s OMNIWeb ( https://omniweb.gsfc.nasa.gov ).

Authors=Ferradas, C. P.; Thaller, S. A.; Fok, M. -C.; Reeves, G. D.; Larsen, B. A.;Title=The Influence of the Inner Magnetospheric Electric Field on Plasma Sheet Access, 2024, doi:10.1029/2024JA033030, ID:32032745.Keywords: space physics data facility, omni, omniwebSample usage ( BODY ) =We acknowledge use of the Kp index from the OMNI data set obtained through NASA/GSFC’s Space Physics Data Facility’s OMNIWeb service.Sample usage ( BODY ) =We acknowledge use of the Kp index from the OMNI data set obtained through NASA/GSFC’s Space Physics Data Facility’s OMNIWeb service.

Authors=Hosokawa, K.; Miyoshi, Y.; Mcharg, M.; Ledvina, V.; Hampton, D.; Lessard, M.; Shumko, M.; Asamura, K.; Sakanoi, T.; Mitani, T.; Namekawa, T.; Nose, M.; Ogawa, Y.; Jaynes, A.; Halford, A.;Title=Variation of the Altitude of Auroral Emission During a Substorm Cycle: Stereoscopic Optical Observations During the LAMP Rocket Experiment, 2024, doi:10.1029/2024JA033036, ID:32032746.Keywords: omniSample usage ( BODY ) =The IMF By and Bz taken from the OMNI database (Figures 2a and 2b) indicate enhanced fluctuations in the magnetic field which started at ~2 days before the launch.

Authors=Zhang, Kun; Artemyev, Anton V.; Li, Xinlin; Zhang, Xiao-Jia; Angelopoulos, Vassilis; Mei, Yang; Xiang, Zheng; Grimmich, Niklas;Title=Nightside Electron Precipitation Patterns as Observed by ELFIN and CIRBE CubeSats, 2024, doi:10.1029/2024JA033051, ID:32032747.Keywords: cdawebSample usage ( BODY ) =NOAA/POES and GOES data used in this study are publicly available at https://cdaweb.gsfc.nasa.gov. GEO-KOMPSAT-2A (SOSMAG) data are made available via ESA’s Space Safety Programme and its provision forms part of the ESA Space Weather Service System at https://swe.ssa.esa.int.

Authors=Chen, Jiawen; Zhong, Jiahao; Cai, Xuguang; Hao, Yongqiang; Cai, Lei; Wan, Xin; Li, Qiaoling; Tang, Zijing; Song, Xingyan; Han, Hao; Kuai, Jiawei; Cai, Lujin;Title=Characteristics of Longitudinal Discontinuity Over Nighttime Equatorial Ionization Anomaly Crests With Multiple Observations, 2024, doi:10.1029/2024JA033133, ID:32032751.Keywords: cdawebSample usage ( BODY ) =(b) COSMIC-2 ionPrf: https://tacc.cwa.gov.tw/data-service/fs7rt_trops/level2/ionPrf/ , ivmL2m: https://tacc.cwa.gov.tw/data-service/fs7rt_tdpc/level2/ivmL2m/ , (c) ICON: https://cdaweb.gsfc.nasa.gov/pub/data/icon/l2/ , for IVM (L2-7 Ionospheric Parameters, Version 006), MIGHTI (L2-2 Vector Winds, Version 005), and FUV night (L2-5 Nighttime O + profile, Version 005).

Authors=Godfrey, T. M.; LaBelle, J.;Title=Direction Finding Studies of Simultaneous Auroral 2fce and 3fce Roar Cyclotron Harmonic Radio Emissions, 2024, doi:10.1029/2024JA033162, ID:32032754.Keywords: iri, international reference ionosphereSample usage ( BODY ) =The dashed lines use the electron density profile generated directly by IRI-2020, and the solid lines show the same electron density profile, but multiplied by a factor of 0.8. Sample usage ( BODY ) =PHaRLAP utilizes the newest available version of the International Reference Ionosphere (IRI-2020) model as a function of height and range for a selected location, time, and yearly mean sunspot number (Bilitza et al., 2022).

Authors=Resende, L. C. A.; Zhu, Y.; Santos, A. M.; Chagas, R. A. J.; Denardini, C. M.; Arras, C.; Silva, L. A.; Nogueira, P. A. B.; Chen, S. S.; Andrioli, V. F.; Moro, J.; Costa, J. R.; Li, H.; Wang, C.; Liu, Z.;Title=Nocturnal Sporadic Cusp-Type Layer (Esc) Resulting From Anomalous Excess Ionization Over the SAMA Region During the Extreme Magnetic Storm on 11 May 2024, 2024, doi:10.1029/2024JA033167, ID:32032755.Keywords: omniwebSample usage ( ACK ) =The authors thank Embrace/INPE for providing Digisonde data, OMNIWeb for providing the interplanetary medium data at L1 Lagrangian point, and SuperMAG and WDC Kyoto for providing the magnetic indices SME and SYM-H, respectively.Sample usage ( BODY ) =The interplanetary medium conditions at the L1 Lagrangian point were obtained from OmniWeb database ( https://omniweb.gsfc.nasa.gov/index.html ), and the SME and SYM-H indices were derived from magnetometers data and available at https://supermag.jhuapl.edu/indices and https://wdc.kugi.kyoto-u.ac.jp , respectively. 2 Figure Three-days overview of interplanetary conditions and ground-based magnetic indices from May 10 to 12, 2024, (a) The interplanetary magnetic field component B z , (b) the magnetopause standoff distance R mp , (c) the SME index, and (d) the SYM-H index.

Authors=Janda, B.; Nemec, F.; Nemecek, Z.; Safrankova, J.;Title=Dawn-Dusk Asymmetry of the Magnetopause Distance Under the Parker Spiral Configuration of the IMF, 2024, doi:10.1029/2024JA033181, ID:32032756.Keywords: cdaweb, omniSample usage ( BODY ) =Data Availability Statement The used magnetic field and plasma data can be accessed from open-access sources via http://cdaweb.gsfc.nasa.gov/cdaweb. The SPACE resource description of the used 5-min OMNI data can be found at Papitashvili and King ( 2020). Sample usage ( BODY ) =The corresponding solar wind parameters are attributed to each of the magnetopause crossings using the 5-min OMNI data. These data are based on measurements from several solar wind monitoring spacecraft around the Lagrange L1 point and are time-shifted to the expected arrival times at the bow shock nose (Papitashvili King, 2020). The solar wind parameters considered include the three components of the IMF and dynamic pressure. Crossings with missing OMNI data are discarded. These criteria result in a total of 42,175 magnetopause crossings for our analysis. 1 Figure Locations of the analyzed magnetopause crossings in the r - x $\rho -x$ plane, where the x $x$ axis is oriented opposite to the incoming solar wind, and r = y 2 + z 2 $\rho =\sqrt{{y}^{2}+{z}^{2}}$ denotes the distance from the x $x$ axis.

Authors=Tsyganenko, N. A.; Semenov, V. S.; Erkaev, N. V.; Gubaidulin, N. T.;Title=Magnetosheath Plasma Flow and Its Response to IMF and Geodipole Tilt as Obtained From the Data-Based Modeling, 2024, doi:10.1029/2024JA033233, ID:32032760.Keywords: cdaweb, spdf, omni, omniwebSample usage ( ACK ) =In particular, Cluster and MMS magnetometer/ephemeris data were obtained from the NSSDC CDAWEB online facility, originally made available by the PIs: A. Balogh and M. Sample usage ( BODY ) =Data Availability Statement Cluster, THEMIS, and MMS magnetometer and plasma instrument data were downloaded from the NSSDC CDAWEB interface at https://cdaweb.gsfc.nasa.gov/cdaweb/index.html. One-minute resolution OMNI data were obtained from SPDF OMNIWEB at https://omniweb.gsfc.nasa.gov. Sample usage ( ACK ) =High-resolution OMNI interplanetary data were obtained from the SPDF OMNIWEB interface (R. McGuire, N. Papitashvili). The authors acknowledge financial support from the Russian Science Foundation Grant 23-47-00084 “Magnetic Reconnection in Space and Laboratory Plasmas: Computer Simulations and Empirical Modeling. All data sets and software used to obtain the above described results are freely available from the FigShare repository at https://doi.org/10.6084/m9.figshare.27282336.v1. Sample usage ( ACK ) =McFadden are acknowledged for the use of THEMIS FGM and ESA data. Sample usage ( BODY ) =At the same time, it should be realized that the modeling results represent only an average picture, derived from data taken at different times and additionally blurred with inaccuracies in the interplanetary OMNI data due to uncertainties of the propagation time/path from L1 to the Earth’s bow shock (e.g., Vokhmyanin et al., 2019). Sample usage ( ABSTRACT ) =The spacecraft data pool includes 1-min average data by Themis (2007-2024), Cluster (2001-2022), and MMS-1 (2015-2024) missions, as well as OMNI interplanetary data. The model drivers include the solar wind particle flux, IMF components, and the geodipole tilt angle.

Authors=Huang, Fuqing; Lei, Jiuhou; Zhang, Shun-Rong; Wang, Yihan; Li, Zhongli; Zhong, Jiahao; Yan, Rui; Aa, Ercha; Zhima, Zeren; Luan, Xiaoli;Title=Peculiar Nighttime Ionospheric Enhancements Over the Asian Sector During the May 2024 Superstorm, 2024, doi:10.1029/2024JA033350, ID:32032761.Keywords: omniwebSample usage ( BODY ) =The CSES data is funded by the China National Space Administration (CNSA) and China Earthquake Administration (CEA), which can be downloaded from the website ( https://www.leos.ac.cn ). We acknowledge OMNIWeb ( https://omniweb.gsfc.nasa.gov/ ) for the geomagnetic data. The authors acknowledge the data resources from the National Space Science Data Center, National Science and Technology Infrastructure of China ( http://www.nssdc.ac.cn/eng/ ).

Authors=Zhao, Yingying; Zhu, Hui;Title=Test Particle Simulations of the Butterfly Distribution of Relativistic Electrons in Magnetic Dips, 2024, doi:10.1029/2024JA032546, ID:32032771.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement The Van Allen Probe data are available at https://cdaweb.gsfc.nasa.gov/pub/data/rbsp/rbspb/ .

Authors=Maletckii, B.; Astafyeva, E.;Title=Near-Real-Time Identification of the Source of Ionospheric Disturbances, 2024, doi:10.1029/2024JA032664, ID:32032779.Keywords: space physics data facility, omni, omniweb, iriSample usage ( BODY ) =The authors acknowledge the NASA/GSFC’s Space Physics Data Facility’s OMNIWeb service ( https://omniweb.gsfc.nasa.gov/ ; Data Page— https://omniweb.gsfc.nasa.gov/form/omni_min.html ) for the data of the interplanetary and geophysical parameters and the World Data Center for Geomagnetism in Kyoto (WDC-Kyoto, http://wdc.kugi.kyoto-u.ac.jp/ ; Data Page— https://wdc.kugi.kyoto-u.ac.jp/wdc/Sec3.html ) for the data of AE index for the 7 October 2015 Storm. Sample usage ( BODY ) =Based on the sound speed profile (Figure 16a), the CSID would take ~8.5 min to reach the altitude maximum ionization altitude of 300 km (according to IRI-2016 (Bilitza et al., 2017), red line) and to ~250 km according to the JJ433 ionosonde, green line).

Authors=Wang, Xu; Dai, Lei; Yong, Ren; Xiong, Senlin; Wang, Chi;Title=The Evolution of Earth’s Outer Radiation Belt Over Geomagnetic Storm Phase in Van Allen Probe Era, 2024, doi:10.1029/2024JA032674, ID:32032780.Keywords: cdaweb, omni, omniwebSample usage ( BODY ) =Data and Processing Method Data In this work, we identify 196 storm events between October 2012 and September 2019 using 1 min SYM-H index from the OMNI database ( http://cdaweb.gsfc.nasa.gov/ ). The storm events are listed in Table 1. The minimum of SYM-H S Y M - H min $\left(SYM-{H}_{\min }\right)$ is required to be less than -40 nT for storm selections. The storm events are listed in Table 1. Sample usage ( BODY ) =Geomagnetic index data is available at https://omniweb.gsfc.nasa.gov/ .

Authors=Han, Shin-Chan; Kil, Hyosub; Ray, Richard; Lemoine, Frank; Waters, Colin;Title=Detection of Extensive Equatorial Plasma Depletions After the 2022 Tongan Volcanic Eruption From Multiple Geodetic Satellite Ranging Systems, 2024, doi:10.1029/2024JA032690, ID:32032781.Keywords: iri, international reference ionosphereSample usage ( BODY ) =In these profiles, the minimum value of GPS estimates was matched to that of the International Reference Ionosphere (IRI) model values (Bilitza, 2018). 1 Figure CubeSat GPS measurements of electron density (Ne) changes.

Authors=Chen, Yiding; Liu, Libo; Le, Huijun; Zhang, Ruilong;Title=Martian Ionosphere-Thermosphere Coupling in Longitude Structures: Statistical Results for the Main Ionization Peak Height, 2024, doi:10.1029/2024JA032839, ID:32032785.Keywords: omniwebSample usage ( BODY ) =The F 10.7 index can be obtained from the OMNIWeb at https://omniweb.gsfc.nasa.gov/form/dx1.html.

Authors=He, Zhaohai; Xu, Jiyao; Dai, Lei; Duan, Suping; Gao, Hong; Wang, Guojun; Roth, Ilan; Wang, Chi;Title=Solar Activity Effects on the Near-Earth Space Regions During the Descending Phase of Solar Cycle 24, 2024, doi:10.1029/2024JA032860, ID:32032789.Keywords: cdawebSample usage ( BODY ) =The solar wind conditions (IMF Bz, flow speed, and proton density), AL and SYM-H indices are obtained from https://cdaweb.gsfc.nasa.gov/cgi-bin/eval1.cgi. There exist two methods to determine the locations of plasmapause, including the density gradient method which is defined as a variation of density by a factor 5 within half L for each half-orbit (Carpenter Anderson, 1992; Zhang et al., 2017) and the density threshold method which is defined by the L shell at a density threshold of ~100 cm -3 following Carpenter ( 1966).

Authors=Tsurutani, Bruce T.; Hajra, Rajkumar; Lakhina, Gurbax; Meng, Xing;Title=Revisiting the Superstorm on 6-7 April 2000 Caused by an Extraordinary Corotating Interaction Region (With an Embedded Coronal Jet?), 2024, doi:10.1029/2024JA032989, ID:32032797.Keywords: omni, omniwebSample usage ( BODY ) =The 1-min solar wind and interplanetary magnetic field (IMF) data are the upstream solar wind measurements shifted to the Earth’s bow shock nose, obtained from NASA’s OMNI website ( https://omniweb.gsfc.nasa.gov/ ). The ring current indices SYM-H (1-min resolution) and Dst (1-hr) are obtained from the World Data Center for Geomagnetism, Kyoto, Japan (WDC; https://wdc.kugi.kyoto-u.ac.jp/ ). The ring current indices SYM-H (1-min resolution) and Dst (1-hr) are obtained from the World Data Center for Geomagnetism, Kyoto, Japan (WDC; https://wdc.kugi.kyoto-u.ac.jp/ ).

Authors=Vaishnav, Rajesh; Jacobi, Christoph; Schmolter, Erik; Duhnen, Hanna;Title=Influence of Lower Atmospheric Variability: An Investigation of Delayed Ionospheric Response to Solar Activity, 2024, doi:10.1029/2024JA032999, ID:32032799.Keywords: spdf, omniwebSample usage ( BODY ) =The TIEGCM simulation data used for this work can be accessed at https://spdf.gsfc.nasa.gov/pub/data/icon/l4/ (NASA, 2024d).Sample usage ( BODY ) =Daily Kp indices have been downloaded from https://omniweb.gsfc.nasa.gov/form/dx1.html (NASA, 2024c). The F10.7 index at 1 AU have been obtained from the LISIRD database (LASP, 2024a, https://lasp.colorado.edu/lisird/ ).

Authors=Singh, Ram; Scipion, Danny E.; Kuyeng, Karim; Condor, Percy; De La Jara, Cesar; Velasquez, Juan Pablo; Flores, Roberto; Ivan, Edwar;Title=Ionospheric Disturbances Observed Over the Peruvian Sector During the Mother’s Day Storm (G5-Level) on 10-12 May 2024, 2024, doi:10.1029/2024JA03300310.22541/essoar.172108210.04033367/v1, ID:32032800.Keywords: cdaweb, omni, omniwebSample usage ( ACK ) =We thank NASA/GSFC for permitting us access to the OMNIWeb (CDAWeb) service and the OMNI data used in this study. We also thank the GPS-TEC data provided by the Madrigal database and the online archives of the Crustal Dynamics Data Information System (CDDIS) of the NASA Goddard Space Flight Canter. Sample usage ( BODY ) =Geomagnetic (e.g., Kp index, Sym-H) and interplanetary solar wind (e.g., IMF B, solar wind speed, particle density) parameters are taken from Advance Composition Explorer (ACE) satellite measurements from the CDAWeb ( https://cdaweb.gsfc.nasa.gov/ ). Observation and Results Figure 1 displays the interplanetary and geomagnetic conditions measured by the ACE spacecraft at the L1 point during the Mother’s Day storm on 10-12 May 2024.

Authors=Hao, Y. -X.; Shprits, Y. Y.; Menietti, J. D.; Liu, Z. Y.; Averkamp, T.; Wang, D. D.; Kollmann, P.; Hospodarsky, G. B.; Drozdov, A.; Roussos, E.; Krupp, N.; Horne, R. B.; Woodfield, E. E.; Bolton, S. J.;Title=Jupiter’s Whistler-Mode Belts and Electron Slot Region, 2024, doi:10.1029/2024JA03285010.22541/essoar.171052479.93456522/v1, ID:32505146.Keywords: omniSample usage ( BODY ) =Solid curves present median values of wave intensity in each frequency bin (colored) and total integrated wave intensity (black). (b) Median omni-directional electron differential fluxes against M-shell measured near the magnetic equator.

Authors=Chaston, C. C.;Title=Energy Transport and Conversion Above a Bright Discrete Auroral Arc, 2024, doi:10.1029/2024JA032870, ID:32505150.Keywords: omniSample usage ( BODY ) =(j-k) Velocity space distributions for electrons in differential energy flux, omni-directional phase space density and ion differential energy flux respectively.

Authors=Wang, Yuhan; Ren, Zhipeng; Liu, Yunbo;Title=A Quiet-Day Ionospheric Electrodynamics Empirical Model in the Low and Middle Latitudes, 2024, doi:10.1029/2024JA032937, ID:32505153.Keywords: space physics data facility, iri, international reference ionosphereSample usage ( BODY ) =The geomagnetic index and solar activity index can be downloaded from the Space Physics Data Facility website ( https://stereo-ssc.nascom.nasa.gov/ ). Sample usage ( BODY ) =The drift model based on ROCSAT-1 by Fejer et al. ( 2008) has been included in international reference ionosphere (IRI). The electric field morphology of the ionospheric F-layer in the low latitudes was described in detail in the reviews by Fejer ( 1981, 1991, 2002, 2011). The electric field morphology of the ionospheric F-layer in the low latitudes was described in detail in the reviews by Fejer ( 1981, 1991, 2002, 2011).

Authors=Pitzel, Jared C.; Cully, Christopher M.; Ripoll, Jean-Francois; Loridan, Vivien; Huang, Chia-Lin; Spence, Harlan E.; Reeves, Geoff D.; Murphy, Kyle R.;Title=Derivations of the Total Radiation Belt Electron Content, 2024, doi:10.1029/2024JA032940, ID:32505154.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement The Van Allen Probes flux data is available through the Coordinated Data Analysis Web (CDAWeb), or directly from the Los Alamos National Laboratory (LANL), at https://cdaweb.gsfc.nasa.gov/ and https://rbsp-ect.newmexicoconsortium.org/data_pub/ respectively.

Authors=Patgiri, D.; Nirwal, S.; Rathi, R.; Yadav, V.; Sunil Krishna, M. V.; Kannaujiya, S.; Sunda, S.; Liu, Jann-Yenq; Sarkhel, S.;Title=Role of Coupled Electrodynamics of E- and F-Regions on the Rapid Poleward Extension of EMSTID Fronts, 2024, doi:10.1029/2024JA032991, ID:32505158.Keywords: cdawebSample usage ( BODY ) =The Level 2.2 (version 5) cardinal wind data of ICON MIGHTI are available at https://cdaweb.gsfc.nasa.gov/pub/data/icon/. The SNR profiles (caL1Snr of level 1b) of FORMOSAT 7/COSMIC-2 are available at CDAAC: COSMIC Data Analysis and Archive Center: https://www.cosmic.ucar.edu/what-we-do/cosmic-2/data/ .

Authors=Gao, Shunzu; Xiong, Chao; Zhu, Ziyuan; Zhan, Weijia; Pignalberi, Alessio; Zhang, Hong;Title=Altitudinal Variation of O+ Scale Height at the Equatorial Topside Ionosphere, 2024, doi:10.1029/2024JA033033, ID:32505159.Keywords: space physics data facility, omniweb, iri, international reference ionosphereSample usage ( BODY ) =Data Availability Statement The authors acknowledge the CEDAR madrigal database ( http://cedar.openmadrigal.org/ ) for providing ISR profile data (by registering your personal information, and searching for “Incoherent Scatter Radars Instruments” in the box of “Choose instrument category(s)” and “Jicamarca IS Radar” in the box of “Choose instrument(s)”, then clicking the “list experiments”), the Space Physics Data Facility at Goddard Space Flight Center ( https://omniweb.gsfc.nasa.gov/ ) for providing Kp and F10.7 indices data. The SAMI2 modeled values are generated using sami2py 0.2.5 (Klenzing et al., 2021, 2022). Sample usage ( BODY ) =Among these studies, the altitude-dependent scale height method has become the mostly used choice for many empirical models, such as the International Reference Ionosphere model (IRI) and the NeQuick model (Bilitza et al., 2017, 2022; Nava et al., 2008; Olivares-Pulido et al., 2016).

Authors=Adhitya, P.; Bulusu, Jayashree; Nose, Masahito; Vichare, Geeta; Dimri, A. P.;Title=Statistics of Higher Harmonics SRS at Low Latitude Station, Shillong, 2024, doi:10.1029/2024JA033034, ID:32505160.Keywords: omniweb, iri, vitmoSample usage ( BODY ) =Geomagnetic field data from the IGRF model can be obtained at https://omniweb.gsfc.nasa.gov/vitmo/cgm.html. Sunspot data is obtained from the World Data Center SILSO, Royal Observatory of Belgium, Brussels ( https://www.sidc.be/SILSO/datafiles#total ). Sample usage ( BODY ) =The data of ion composition and electron density required to calculate the Q factor is obtained from IRI-2016 model, whereas the height integrated conductivity is obtained from WDC Kyoto. Sample usage ( BODY ) =Geomagnetic field data from the IGRF model can be obtained at https://omniweb.gsfc.nasa.gov/vitmo/cgm.html. Sunspot data is obtained from the World Data Center SILSO, Royal Observatory of Belgium, Brussels ( https://www.sidc.be/SILSO/datafiles#total ).

Authors=Nie, Wenfeng; Wang, Fangyuan; Qiao, Zhizhong; Xu, Tianhe; Wang, Yong; Ye, Mingzhu; Hu, Lianhuan; Liu, Tong;Title=Ionospheric Irregularities Coinciding With the 2023 Typhoon Saola: A Multi-Instrument Study, 2024, doi:10.1029/2024JA033043, ID:32505161.Keywords: cdaweb, omniwebSample usage ( BODY ) =The IMF data are provided from CDAWeb at https://cdaweb.sci.gsfc.nasa.gov/. The F10.7 measurement and Dst are provided by the Goddard Space Flight Center (GSFC) from https://omniweb.gsfc.nasa.gov/. Sample usage ( BODY ) =The F10.7 measurement and Dst are provided by the Goddard Space Flight Center (GSFC) from https://omniweb.gsfc.nasa.gov/. Tropical Cyclone Data The data on tropical cyclones is from the global real-time satellite cloud image website ( https://rammb-data.cira.colostate.edu/tc_realtime/ , namely RAMMB in NOAA).

Authors=Sun, Yu; Wang, Hui; Zhang, Kedeng;Title=Impact of Interplanetary Magnetic Field By on Subauroral Polarization Streams at Dawn and Dusk, 2024, doi:10.1029/2024JA033063, ID:32505162.Keywords: space physics data facility, omniwebSample usage ( BODY ) =The solar wind and interplanetary magnetic field and magnetic activity index data are from NASA/GSFC’S Space Physics Data Facility’s OMNIWeb ( https://omniweb.gsfc.nasa.gov ).

Authors=Zhang, Ruilong; Liu, Libo; Yang, Yuyan; Li, Wenbo; Zhao, Xiukuan; Yoshikawa, Akimasa; Tariq, M. Arslan; Chen, Yiding; Le, Huijun;Title=Ionosphere Responses Over Asian-Australian and American Sectors to the 10-12 May 2024 Superstorm, 2024, doi:10.1029/2024JA033071, ID:32505163.Keywords: cdaweb, omniSample usage ( BODY ) =Observations The solar wind and F10.7 data are from the OMNI database ( https://cdaweb.gsfc.nasa.gov/pub/data/omni/ ). The Dst index is obtained from the Word Data Center for Geomagnetism, Kyoto ( https://wdc.kugi.kyoto-u.ac.jp/dst_realtime/202405/index.html ).

Authors=Fok, M. -C.; Wolf, R. A.; Ferradas, C. P.; Kang, S. -B.; Glocer, A.; Buzulukova, N. Y.; Ma, Q.; Welling, D. T.;Title=Implementation of an Asymmetric Internal Field in the Comprehensive Inner Magnetosphere-Ionosphere (CIMI) Model, 2024, doi:10.1029/2024JA033075, ID:32505164.Keywords: cdaweb, omni, omniwebSample usage ( BODY ) =The solar wind data as input to the CIMI model are from Wind and publicly available through the Coordinated Data Analysis Web (CDAWeb) at https://cdaweb.gsfc.nasa.gov. The AE, Kp, and Dst indices, also input parameters for the CIMI model, were obtained from the OMNI data set provided by the OMNIWeb service at https://omniweb.gsfc.nasa.gov/. The routines used to calculate the IGRF magnetic field are taken from the Geopack 2008, which can be downloaded from https://geo.phys.spbu.ru/~tsyganenko/empirical-models/coordinate_systems/geopack/.

Authors=Yadav, Sneha; Lyons, Larry R.; Nishimura, Yukitoshi; Liu, Jiang; Tian, Sheng; Zou, Ying; Donovan, Eric F.;Title=Investigating the Spatiotemporal Development of Substorm Expansion Phase Aurora: Successive Onsets or Poleward Boundary Intensifications?, 2024, doi:10.1029/2024JA033086, ID:32505166.Keywords: cdaweb, spdf, omni, omniwebSample usage ( BODY ) =Data Availability Statement THEMIS data can be obtained online at https://cdaweb.gsfc.nasa.gov/pub/data/themis/. SuperMAG ground magnetometer and SML data can be obtained at supermag.jhuapl.edu. Sample usage ( BODY ) =Solar wind parameters (IMF Bz) were obtained from the SPDF, NASA, USA at http://omniweb.gsfc.nasa.gov. Space Physics Environment Data Analysis Software (SPEDAS) tool, which is used to download and analyze the data, can be downloaded from https://spedas.org/blog/. Sample usage ( BODY ) =The solar wind parameters (interplanetary magnetic field (IMF) Bz, By) are obtained from the OMNI database. We used the SuperMAG auroral indices SML (analogous to AL, Gjerloev, 2012; Newell Gjerloev, 2011) at a 1-min cadence. Space Physics Environment Data Analysis Software (SPEDAS) tool, which is used to download and analyze the data, can be downloaded from https://spedas.org/blog/.

Authors=Huang, Sheng; Li, Wen; Ma, Qianli; Shen, Xiao-Chen; Capannolo, Luisa; Chu, Xiangning;Title=Modeling Global Electron Precipitation Driven by Whistler Mode Waves: Integrating Physical and Deep Learning Approaches, 2024, doi:10.1029/2024JA033089, ID:32505168.Keywords: omniwebSample usage ( BODY ) =Geomagnetic indices used in model training, including SYM-H, were accessed from NASA’s OMNIWeb (Papitashvili et al., 2020). The SML and SMU indices (Newell Gjerloev, 2011) were accessed through the SuperMAG service (Gjerloev, 2012), and the Hp30 index (Matzka et al., 2022) was obtained from the GFZ Potsdam archive.

Authors=Sun, Wenjie; Li, Guozhu; Zhang, Shun-Rong; Zhao, Biqiang; Li, Yu; Tariq, M. Arslan; Zhao, Xiukuan; Hu, Lianhuan; Dai, Guofeng; Xie, Haiyong; Li, Yi; Liu, Jianfei; Ning, Baiqi; Liu, Libo;Title=Complex Ionospheric Fluctuations Over East and Southeast Asia During the May 2024 Super Geomagnetic Storm, 2024, doi:10.1029/2024JA033096, ID:32505169.Keywords: omniSample usage ( BODY ) =Figure 1 presents the solar wind speed measured by the ACE satellite that was post-processed and archived in the OMNI database ( https://spdf.gsfc.nasa.gov/pub/data/**omni**/high_res_omni/ ), Dst/SYM-H ( https://wdc.kugi.kyoto-u.ac.jp/ ) and Kp ( https://kp.gfz-potsdam.de/en/ ) indices during 09-13 May 2024.

Authors=Shukhtina, M. A.; Sergeev, V. A.; Nikolaev, A. V.; Artemyev, A.; Angelopoulos, V.; Rodriguez, J. V.;Title=Magnetic Dipolarizations and Energetic Electron Flux Variations at the Nightside Geostationary Orbit, 2024, doi:10.1029/2024JA033097, ID:32505170.Keywords: cdaweb, omniSample usage ( BODY ) =Data Availability Statement The magnetic field and MAGED data was obtained from the site Index of/instruments/solar-space-observing/particle-detectors/sem/goes/access/avg and from https://cdaweb.gsfc.nasa.gov/index.html . The MPB index is available at Chu, X. ( 2021). Sample usage ( BODY ) =AL and AE indices were taken from OMNI data base, https://cdaweb.gsfc.nasa.gov/cgibin/eval2 .

Authors=Starkey, M. J.; Fuselier, S. A.; Dayeh, M. A.;Title=Conditions of High Helium Concentrations in Coronal Mass Ejections, 2024, doi:10.1029/2024JA033099, ID:32505171.Keywords: spdf, omni, omniwebSample usage ( BODY ) =Data Availability Statement Wind data were obtained from the GSFC/SPDF OMNIWeb interface at http://omniweb.gsfc.nasa.gov .Sample usage ( BODY ) =Epoch Analysis of Sym-H To investigate the effect of high-concentration events on Earth’s geomagnetic activity, we perform an epoch analysis of the 1-min Sym-H index obtained from the OMNI database. For each event, we obtain the Sym-H time series data for a time window up to 3 days after the Wind observation of the ICME.

Authors=Xia, Hao; Wang, Hui; Zhang, Kedeng;Title=Extreme Responses of the Ionospheric Radial Currents to the Main Phase of the Super Geomagnetic Storm on 10 May 2024, 2024, doi:10.1029/2024JA033126, ID:32505174.Keywords: omniSample usage ( BODY ) =Data and Model The high-resolution (1 min) OMNI database is a complication made from the records of ACE, WIND, and IMP-8 mission.

Authors=Ranjan, Alok Kumar; Nailwal, Dayakrishna; Sunil Krishna, M. V.; Kumar, Akash; Sarkhel, Sumanta;Title=Evidence of Potential Thermospheric Overcooling During the May 2024 Geomagnetic Superstorm, 2024, doi:10.1029/2024JA03314810.48550/arXiv.2411.14071, ID:32505176.Keywords: omniwebSample usage ( BODY ) =To characterize the geomagnetic superstorm considered in this study, solar wind parameters such as plasma pressure and IMF-Bz (north-south) component, as well as geomagnetic indices (Dst-index, AE-index, ap-index, and polar cap index for Northern hemisphere (PCN-index)) are used with 1 and 3 hr cadence from the OMNIWeb data set (https://omniweb.gsfc.nasa.gov/) and The International Service of Geomagnetic Indices (ISGI) ( https://isgi.unistra.fr/whats_isgi.php ).

Authors=Laskar, F. I.; Pedatella, N. M.; Codrescu, M. V.; Eastes, R. W.; Anderson, J. L.;Title=Assessing the Impacts of Assimilating GOLD Disk O/N2 Observations on the Thermosphere-Ionosphere System, 2024, doi:10.1029/2024JA03316310.22541/essoar.171691251.16694001/v1, ID:32505177.Keywords: space physics data facilitySample usage ( BODY ) =Data Availability Statement GOLD Level 2 data used in this study are available at the GOLD Science Data Center ( https://gold.cs.ucf.edu/search/ ) and at NASA’s Space Physics Data Facility ( https://spdf.gsfc.nasa.gov/pub/data/gold/level2/on2/ ).

Authors=Tripathi, Rajat; Bhaskar, Dayanand; Maurya, Ajeet Kumar; Kumar, Sushil; Singh, Rajesh;Title=Lower Ionospheric Disturbances Due To Geomagnetic Storms of March and April 2023: Inferred From VLF Navigational Signals and Numerical Simulations, 2024, doi:10.1029/2024JA033188, ID:32505183.Keywords: omniwebSample usage ( BODY ) =The Z -component of IMF IMF B Z values were obtained from the OMNIweb portal of NASA ( https://omniweb.gsfc.nasa.gov/form/dx1.html ). 1 Figure The figure shows the transmitter receiver great circle path of two very low frequency transmitters (NWC and VTX) and the receiver in Dehradun (DDN) used in the present study.

Authors=Geethakumari, G. P.; Aikio, A. T.; Cai, L.; Vanhamaki, H.; Virtanen, I. I.; Coster, A.; Marchaudon, A.; Blelly, P. -L.; Maute, A.; Norberg, J.; Oyama, S.; Zhang, Y.; Kunduri, B. S. R.; Title=Total Electron Content Variations During an HSS/SIR-Driven Geomagnetic Storm at High and Mid Latitudes, 2024, doi:10.1029/2024JA033192, ID:32505185.Keywords: cdaweb, space physics data facility, omni, omniwebSample usage ( ACK ) =We acknowledge use of NASA/GSFC’s Space Physics Data Facility’s CDAWeb service and OMNI data for providing magnetic indices and solar wind parameters. We thank the AMPERE team and the AMPERE Science Data Center for providing data products derived from the Iridium Communications constellation, enabled by support from the National Science Foundation. Sample usage ( BODY ) =Data for the solar wind, interplanetary magnetic field (IMF) and geomagnetic indices were taken from the OMNI database (King Papitashvili, 2005) with a cadence of 5 min. In this study,the SYM-H index, a high resolution version of Dst index with a temporal resolution of 1 min (Wanliss Showalter, 2006) is used. Sample usage ( BODY ) =Data for the solar wind, IMF and geomagnetic indices were taken from the OMNI data base at (https://omniweb.gsfc.nasa.gov/form/omni_min.html).

Authors=Salohub, A.; Safrankova, J.; Nemecek, Z.; Pi, G.;Title=A Novel Determination of the Foreshock ULF Boundary: Statistical Approach, 2024, doi:10.1029/2024JA033195, ID:32505186.Keywords: cdaweb, omniSample usage ( BODY ) =Data Availability Statement The magnetic field and plasma data are public and are available online via http://cdaweb.gsfc.nasa.gov/ ; details: THEMIS-ARTEMIS data at cdaweb. gsfc.nasa.gov/pub/data/themis; and the Wind data can be accessed via cdaweb. gsfc.nasa.gov/pub/data/wind, all using the particular instruments and time intervals of events for an identification.Sample usage ( ACK ) =Acknowledgments The authors thank the THEMIS/ARTEMIS, ACE and OMNI database working teams for the magnetic field and plasma data used for the analysis. Sample usage ( BODY ) =THEMIS observations were divided into 10-min intervals and, since the spacecraft visit different regions, we compare magnetic field and plasma parameters with the solar wind values from the OMNI database. We select the intervals in which the mean magnetic field and plasma parameters differ by less than 15 % $15%$ from upstream values.

Authors=Elliott, S. S.; Colpitts, C.; Breneman, A. W.; Pettit, J. M.; Cantwell, K. A.; Cattell, C. A.; Halford, A. J.; Shumko, M.; Sample, J.; Johnson, A.; Miyoshi, Y.; Kasahara, Y.; Troyer, R. N.; Millan, R.; Hori, T.; Shinohara, I.; Matsuda, S.; Matsuoka, A.; Title=A Multi-Platform Statistical Analysis of the Azimuthal Spatial Extent of the Microburst Precipitation Region, 2024, doi:10.1029/2024JA033208, ID:32505187.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement Data—Science data of the Van Allen Probes (RBSP) used in this study can be found on the Coordinated Data Analysis Web (CDAWeb) ( https://cdaweb.gsfc.nasa.gov/ ) (EFW data is also available on http://www.space.umn.edu/rbspefw-data/ and EMFISIS on https://emfisis.physics.uiowa.edu/data/index ), see Kletzing et al. ( 2013).

Authors=Liu, Terry Z.; Angelopoulos, Vassilis; An, Xin; Madanian, Hadi;Title=ARTEMIS Observations of Lunar Crustal Field-Solar Wind Interaction and Impact on Reflected Plasma Under Weak Radial IMF, 2024, doi:10.1029/2024JA033217, ID:32505188.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement ARTEMIS data set are available at NASA’s Coordinated Data Analysis Web (CDAWeb, http://cdaweb.gsfc.nasa.gov/ ). The SPEDAS software (see Angelopoulos et al. ( 2019)) is available at http://themis.ssl.berkeley.edu.

Authors=Jiang, Y. C.; Chen, Z. Z.; Yu, J.; Wang, J.; Liu, X. M.; Cui, J.; Cao, J. B.; Ren, A. J.; Ding, X. L.;Title=Low-Frequency Whistler Waves Excited by Electron Butterfly Distributions in Turbulent Reconnection Outflow, 2024, doi:10.1029/2024JA033250, ID:32505193.Keywords: omniSample usage ( BODY ) =Due to the neglect of the effects of the kappa distribution (Summers Tang, 2021), slight adjustments may be necessary for the dispersion relation. 1 Table Fitting Parameters of Electron Phase Space Densities by Using Multiple Bi-Maxwellian Distribution Functions n e [cm -3 ] T e // [eV] T e [eV] V b [km/s] 1 0.15 6 6 0 2 0.19 800 800 0 3 0.02 2700 2700 0 4 0.20 300 600 9000 5 0.20 350 600 -9000 To reveal the properties of the resonant electrons, Figure 4 presents the averaged omni-directional PSD as a function of electron energy during the interval 04:33:31.800-04:33:32.200 UT.

Authors=Zhang, Kedeng; Wang, Hui; Liu, Jing; Song, Huimin; Liu, Xuanqing;Title=The Significant Enhanced Quiet-Time Equatorial Ionization Anomaly by the Intense Solar Flare on 06 September 2017, 2024, doi:10.1029/2024JA033264, ID:32505195.Keywords: cdaweb, omniSample usage ( BODY ) =The solar wind data is downloaded from OMNI ( https://cdaweb.gsfc.nasa.gov/index.html ), and the Kp index can be found in WDC ( https://wdc.kugi.kyoto-u.ac.jp/kp/index.html#LIST ).

Authors=Nitti, S.; Carter, J. A.; Sembay, S. F.; Milan, S. E.; Zhao, L.; Lepri, S. T.; Kuntz, K. D.;Title=Can XMM-Newton Be Used to Track Compositional Changes in the Solar Wind?, 2024, doi:10.1029/2024JA033323, ID:32505197.Keywords: cdaweb, omni, omni-2, omniwebSample usage ( BODY ) =We believe this discrepancy is caused by the different versions of the ACE data set being used, with ours being publicly available from CDAWeb and Zhao’s the pre-distributed data set available to the instrument team. Sample usage ( ACK ) =The authors are grateful to the National Space Science Data Centre for the ACE and OMNI data, and to the National Oceanic and Atmospheric Administration (NOAA) for the sunspot number data.Sample usage ( BODY ) =We shifted all the data from L1 to Earth, using the time-shifting equation from the OMNI 2 data set on the OMNIWeb page ( https://omniweb.gsfc.nasa.gov/html/ow_data.html ). This approach provides a good approximation of the data time-shift with an accuracy of a few minutes, which is suitable given the time resolution of the ACE data set.

Authors=Zhang, Duan; Zhang, Q. -H.; Oksavik, K.; Tang, B. -B.; Zhang, Y. -L.; Lockwood, M.; Foster, J. C.; Zhang, S. -R.; Lyons, Larry R.; Xing, Z. -Y.; Wang, Yong; Ma, Y. -Z.;Title=A “Wave-Like” Evolution of Polar Cap Patches Modulated by Enhanced Magnetopause Reconnection and Extended Magnetotail Reconnection, 2024, doi:10.1029/2024JA033349, ID:32505200.Keywords: cdawebSample usage ( BODY ) =Data Availability Statement The solar wind and IMF data from the ACE spacecraft is available at the NASA CDAWeb site via https://cdaweb.gsfc.nasa.gov/sp_phys/data/ace/mag/level_2_cdaweb/mfi_h0/2014/ (NASA, 2024).

Authors=Froystein, Ingeborg; Spicher, Andres; Gustavsson, Bjorn; Oksavik, Kjellmar; Johnsen, Magnar Gullikstad;Title=On the Identification of the Dayside Auroral Region Using Incoherent Scatter Radar, 2024, doi:10.1029/2024JA033361, ID:32505201.Keywords: spdf, omni, omniweb, iriSample usage ( BODY ) =The IMF data were obtained from the GSFC/SPDF OMNIWeb interface at https://omniweb.gsfc.nasa.gov (King Papitashvili, 2005). Sample usage ( BODY ) =Finally, solar wind data were obtained through the OMNI database (King Papitashvili, 2005). Figure 1 summarises the observation platforms for this study. Sample usage ( ACK ) =Simulation results of the NRL MSIS and IRI models have been provided by the Community Coordinated Modeling Center (CCMC) at Goddard Space Flight Center through their publicly available simulation services ( https://ccmc.gsfc.nasa.gov ). Sample usage ( BODY ) =For the ionospheric ion compositions and atmospheric neutral densities the IRI 2016 (Bilitza et al., 2017) and NRLMSIS2.0 (Emmert et al., 2021) models are used, respectively.

Authors=Yang, Chang; Yue, Jiaxu; Yang, Hongming; He, Zhaoguo; Xiao, Fuliang; Zhang, Sai; He, Yihua; Liu, Si; Zhou, Qinghua; Gao, Zhonglei; Jin, Yuyue; Zhao, Hui; Johnston, Archie James;Title=Contribution of EMIC and Chorus Waves to the Formation of the Three-Belt of Ultra-Relativistic Electrons, 2024, doi:10.1029/2024JA033380, ID:32505202.Keywords: cdaweb, spdfSample usage ( BODY ) =Data Availability Statement Data for this research are available at the following websites: http://cdaweb.gsfc.nasa.gov/cdaweb/istp_public/ (geomagnetic activity indices) and https://spdf.gsfc.nasa.gov/pub/data/rbsp/ (Van Allen Probes).

Authors=Huang, Binyi; Chen, Peng; Yao, Yibin; Wang, Rong; Zhang, Yuchen;Title=Validation of Ionospheric Parameters From Electron Density Profiles of FY-3E Satellite Using Ionosonde, GIMs, Satellite Altimetry and Other Occultations, 2024, doi:10.1029/2024JA032590, ID:32505208.Keywords: iri, international reference ionosphereSample usage ( BODY ) =An et al. ( 2019) utilized GNSS, satellite altimetry (SA) and IRI models for multi-source data fusion, resulting in significant accuracy improvements. Sample usage ( ABSTRACT ) =Additionally, we use the International Reference Ionosphere (IRI-2020) to normalize VTEC, eliminating systematic biases due to altitude differences. Sample usage ( BODY ) =Numerous ionospheric models, such as the International Reference Ionosphere (IRI) and NeQuick, exist for calculating ionospheric delays (Chen et al., 2020, 2022; Tariku, 2020).