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These events are responsible for large solar energetic particle events in interplanetary space and are the primary cause of major geomagnetic storms at Earth. The two spacecraft are launched to drift slowly away from the Earth in opposite directions at about 10 degrees per year for the lagging spacecraft and 20 degrees per year for the leading one. Optimal longitudinal separation of about sixty degrees is achieved after two years. Afterwards the separation gradually increases beyond the design lifetime of two years with the possibility of extended mission observations at larger angles. Science instruments selected for STEREO include the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) for extreme ultraviolet (EUV), white-light coronographic, and heliospheric imaging, the STEREO/WAVES (SWAVES) interplanetary radio burst tracker, the In situ Measurements of Particles and CME Transients (IMPACT) investigation for in-situ sampling the 3-D distribution and plasma characteristics of solar energetic particles and the interplanetary magnetic field, and the PLAsma and SupraThermal Ion and Composition (PLASTIC) experiment to measure elemental and charge composition of ambient and CME plasma ions. STEREO data recorded and stored onboard each spacecraft will be downlinked through the NASA Deep Space Network on a daily schedule. Real-time space weather data will be continuously transmitted through a separate beacon system to NASA and non-NASA receiving stations."},{"1":" About STEREO data in COHOWEB STEREO-A and -B data are from the magnetometer of the IMPACT package and from the PLASTIC plasma detector.  Principal Investigators for these packages are Janet Luhmann (UCB) and Antoinette Galvin (UNH), respectively.  Magnetic field  data were obtained as 10-min averages from the UCLA web site at http://aten.igpp.ucla.edu/forms/stereo/ascii_PLASTIC_10m_new.html, courtesy of C.T. Russell.  Proton Fluxes from http://www.srl.caltech.edu/STEREO/.  COHOWeb's magnetic field hourly averages were created at GSFC/SPDF by averaging over the six 10-min averages falling within each hour.  Hourly plasma parameter data, including plasma flow direction angles for STEREO-A but not yet for STEREO B (as of 7/11/2010), were obtained from UNH via http://fiji.sr.unh.edu/1dmax_ascii/."}]},{"MODS":[{"0":" "}]},{"NSSDC_ID":[{"0":"2006-047A"}]},{"ADID_ref":[{"0":" "}]},{"Logical_file_id":[{"0":"sta_coho1hr_merged_mag_plasma_00000000_v01"}]},{"Logical_source":[{"0":"sta_coho1hr_merged_mag_plasma"}]},{"Logical_source_description":[{"0":"Merged hourly magnetic field, plasma, proton fluxes, and ephermis data"}]},{"PI_name":[{"0":"Natasha Papitashvili"}]},{"PI_affiliation":[{"0":"NASA/GSFC"}]},{"Mission_group":[{"0":"STEREO"}]},{"Instrument_type":[{"0":"Magnetic Fields (space)"},{"1":"Plasma and Solar Wind"},{"2":"Ephemeris/Attitude/Ancillary"}]},{"Time_resolution":[{"0":"1 hour"}]},{"LINK_TEXT":[{"0":"COHO dataset"},{"1":"Additional analysis tools for these data from the"}]},{"LINK_TITLE":[{"0":"Documentation"},{"1":"COHOWeb 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