CCSD3ZF0000100000001CCSD3VS00002MRK**001 Vol_Ident: USA_NASA_NSSD_P11B_0001 /* | */ /* The last four digits will be sequential from 0001 to ????. */ Vol_Creation_Date: TBD /* e.g.: 1991-??-?? */ /* | */ Medium_Description: 1/2 inch, 9 track, 6250 bpi magnetic tape, unlabeled Technical_Contact: Gordon A. Lentz University of Chicago Enrico Fermi Institute Laboratory for Astrophysics and Space Research 933 E. 56th Street Chicago, IL 60637 Telephone: (312) 702-7836 E-Mail: (NSI/DECnet) LASR::LENTZ : (Internet) lentz@odysseus.uchicago.edu Prev_Vols: none /* | */ /* or some or all of USA_NASA_NSSD_P11B_0001 USA_NASA_NSSD_P11B_0002 */ CCSD$$MARKERMRK**001CCSD3SS00002MRK**002 ************** Material between the *******'s was added in 2009 by Joe King. This documentation file was initially created at U. Chicago in 1993 to describe 15-min-resolution, 6-months-per-file Pioneer 10 and 11 data sets being submitted to NSSDC on magnetic tapes. Tape contents were subsequently put online at NSSDC at ftp://nssdcftp.gsfc.nasa.gov/spacecraft_data/pioneer/pioneer11/ particle/cpi/ip_15min_ascii/ and ftp://nssdcftp.gsfc.nasa.gov/spacecraft_data/pioneer/pioneer11/ particle/cpi/ip_15min_ascii/ Unfortunately, there were no markers (separators) between successive 15-min records, except between the last 15-min record of a day and the first record of the next day. Thus data listings had data for all 96 15-min intervals of a day on one line. In 2009, Natalia Papitashvili (GSFC/SPDF) created new versions of these files, having line-feeds between each pair of 15-min records and also having full-year files rather than 6-month files. Data content was not changed in this process. The newly created files replaced the original files in the above-referenced directories, and new subdirectories ftp://nssdcftp.gsfc.nasa.gov/spacecraft_data/pioneer/pioneer11/ particle/cpi/ip_15min_ascii/old/ and ftp://nssdcftp.gsfc.nasa.gov/spacecraft_data/pioneer/pioneer11/ particle/cpi/ip_15min_ascii/old/ were created in those directories to hold the original files. No other changes have been made in this documentation file to reflect the changes discussed in this addendum. **************** Data_Set_Name: Pioneer 11 CPI Cruise Data Archive Data_Source: Pioneer 11 Charged Particle Instrument Scientific_Contact: Prof. John A. Simpson University of Chicago Enrico Fermi Institute Laboratory for Astrophysics and Space Research 933 E. 56th Street Chicago, IL 60637 Telephone: (312) 702-7670 Spacecraft_Characteristics: The Pioneer 10 and 11 spacecraft are near-twin spacecraft which were launched toward Jupiter about a year apart with different closest-approach radii at the respective encounters, and differing post-encounter trajectories. Pioneer 10 was launched on March 3, 1972, and encountered Jupiter in December, 1973. Since the encounter, it has been on an escape trajectory from the solar system, and at the end of 1991 it was at a distance of about 53 AU from the sun, a celestial latitude of +3 degrees, and a celestial longitude (measured eastward from the vernal equinox) of 73 degrees. Pioneer 11 was launched April 5, 1973 and encountered Jupiter in December 1974. Its post-encounter trajectory was chosen so that it would encounter Saturn some 5 years later; this encounter took place successfully in August-September 1979. At the end of 1991 Pioneer 11 was at a radial distance of 35 AU, a celestial latitude of +17 degrees and a celestial longitude of -95 degrees. Both spacecraft were instrumented with a full suite of instruments for fields and particles, including magnetometer, plasma sensors, and four energetic particle and cosmic ray instruments. Other instruments included an ultraviolet photometer, infrared photometer, imaging photopolarimeter, and micrometeoroid detector. The spacecraft are spin stabilized, with the spin axis oriented toward the earth. Investigation_Objectives: The basic scientific objectives of the University of Chicago Charged Particle Instrument (CPI) on Pioneer 10/11 are divided into two categories: (a) those concerned with studies of the magnetospheric environments of Jupiter (Pioneer 10/11) and Saturn (Pioneer 11 only), and (b) those concerned with investigations in the interplanetary medium. The objectives in the study of the planetary magnetospheres are described in NSSDC documents elsewhere. The interplanetary objectives are directed towards studies of transient and long-term solar modulation of galactic cosmic rays, towards studies of acceleration mechanisms for cosmic rays in interplanetary space, and towards studies of propagation and storage of energetic solar particles, in what can be considered to be three regimes of interplanetary space. These are (1) the inner solar system between one and five A.U. from the Sun, (2) the extended region of the solar cavity beyond the orbit of Jupiter to a predicted terminal shock in the solar wind at 50-150 A.U., and (3) the region between the solar wind termination shock and the 'modulation boundary' at several hundred A.U., expected to be characterized by some kind of transition to the local interstellar medium. The basic interplanetary objectives can be summarized as follows: (1) The measurement of the variation of the differential energy spectra and flux level of energetic charged particles (protons, helium, some heavy nuclei and electrons) with heliographic radius, longitude and latitude, and time. Time variations in the radial and latitudinal gradients are of specific interest for studies of long-term solar modulation of galactic cosmic rays, and the origin of the anomalous components of cosmic rays. The latter is thought to arise from acceleration of cold, singly ionized interstellar atoms at the termination shock of the solar wind. Radial and longitudinal variations are of interest for the study of the propagation of Jovian electrons in the inner heliosphere, where electron acceleration in and leakage from the Jovian magnetosphere is the dominant source, and for the study of cosmic ray particle propagation, acceleration, and transient modulation by traveling shocks and corotating interaction regions. (2) Investigation of the radial and longitudinal dependence of the energy spectra, composition, and time-intensity behavior for energetic particles from solar flares and solar active regions in both the inner and outer heliospheres. Measurements of spatial gradients can be used to determine parameters for energetic particle diffusion parallel and perpendicular to the interplanetary magnetic field, while composition measurements yield information on acceleration and propagation of flare ions within the solar atmosphere and corona. Cruise data are useful for the following reasons in planetary studies: (1) The state of the interplanetary energetic particles can be assessed before the planetary flybys to determine if large solar flare events or effects of interplanetary shock acceleration may inject new particles into the magnetosphere prior to or doing passage through the magnetosphere. (2) Leakage of particles (e.g., Jovian electrons) can be studied as a function of temporal phase with respect to the planetary rotation period to allow inference of the particle source mechanism. In order to meet the interplanetary objectives, continuous measurements of the fluxes, energy spectra, and chemical and isotopic composition of energetic charged particles in the interplanetary medium in the inner and outer heliosphere are required. In particular, for nuclei which stop in the sensors (energy range 0.5 - 67 MeV for protons)the instrument separately identifies individual nuclei including protons, helium and higher Z nuclei up to oxygen, and measures the energy and differential flux of these particles. The integral flux of nuclei which completely penetrate the sensors (energy >67 MeV for protons) is also measured. Electron spectra are measured from ~3 to ~30 MeV. Instrument_Attributes: A. Sensor Characteristics: The Pioneer 10 and 11 CPI instruments consist of four separate sensors, which are the Main Telescope (MT), the Low Energy Subsystem Telescope (LET), the Electron Current Detector (ECD or "Egg"), and the Fission Cell Detector. Detailed descriptions of these sensors are given in Simpson et al. (1974a,b; 1980). For cruise data analysis only the MT and LET telescopes are utilized. 1. The Main Telescope. The major portion of the instrument response is provided by a 7-element solid state telescope utilizing Li-drifted silicon detectors, a CsI scintillator viewed by a photo-diode, and a cylindrical plastic scintillator guard detector viewed by a photomultiplier tube. This detector telescope satisfies the response capability required for the interplanetary objectives given above except as supplemented by the LET sensor described below. Coincidence-anticoincidence requirements on various combinatios of detectors define particle range intervals in which counting rates are measured. In addition, the amount of energy lost in each of three detectors by individual particles passing through the telescope is measured using three pulse height analyzers, thus providing information for particle identification and measurement of energy. The seven detector elements are identified as D1 through D7, where D1, D2, D3, D4, and D6 are Li-drifted silicon detectors, D5 is composed of a CsI scintillator crystal, shaped in the form of a truncated cone, viewed through its bottom face by a Li-drifted silicon photodiode, and D7 is the plastic scintillator. Detectors D1 and D2 are formed as spherical segments in the Pioneer 11 instrument in order to improve resolution. Pioneer 10 had one flat and one curved detector. The so-called "large geometry" of telescope acceptance for incident events is formed by the D1 and D2 detectors which define an acceptance cone of half angle 32 degrees, for which D3 provides a range measurement in this geometry. The "small geometry" is formed by D1 and D4 with a cone half angle of 23 degrees, for which D5 and D6 provide two additional range measurements. The D7 plastic scintillator is used to reject all particles penetrating the configuration from other directions than those defined by the large and small geometries. Coincidence and anticoincidence requirements on combinations of detectors triggered by penetration of a charged particle define particle range intervals (also called range ID's) in which counting rates are measured. In addition to these requirements a restriction requiring the total amount of energy deposited in D1 and D2 to total at least 3 MeV for low-energy counting rates is incorporated in the form of the "slant" or "S" discriminator. This condition eliminates background from gamma rays from 200 keV to 3 MeV produced by the Radio-isotope Thermoelectric Generators (RTG's) which produce power for the spacecraft. Since the sensor electronics are optimized for low flux environments in interplanetary space, the MT coincidence rates are overwhelmed by accidental coincidences in high flux environments, and caution is required in the interpretation of data from such periods (e.g., in Jupiter's magnetosphere or in very large solar flare particle events such as occurred in August 1972). Multiparameter pulse-height analysis is performed using D1, D2, and D5. Energy losses due to charged particle ionization are measured in these three detectors by using multiple-ramp linear post amplifiers in conjunction with 256 channel pulse height analyzers. Hence there are 2 independent streams of digital information: (1) particle event counting rates in the range intervals or ID's, and (2) multiparameter pulse height analysis for each analyzed particle event. The first provides a continuous measure of particle flux, while the second provides information for identifying particle type and energy for a random sample of particles entering the telescope. 2. The Low Energy Telescope. The LET consists of three silicon detectors: a thin (36.3 micron) detector identified as L1, an annular detector, and a flat detector, the last two being coupled together electronically and identified as L2. Passive shielding defines a front aperture of conical half-angle 38 degrees which is further protected by a thin titanium window (0.84 mg/sq-cm) and which points perpendicular to the spacecraft spin axis. The passive shield excludes protons and heavier nuclei below about 45 MeV/amu from penetration to the active detectors from the sides. Protons entering through the aperture trigger only the L1 detector at incident energies of 0.54-1.8 MeV/amu and will trigger both L1 and L2 for energies in the range of 1.8-8.8 MeV/amu. The helium response extends to 50 MeV/amu for L1.L2 events but no heavier ions can be identified. Thirty-two channel pulse height analysis is performed for energy deposition in the L1 detector, which has a 350-keV discriminator threshold. For each L1 event the state of the L2 discriminator is also recorded to identify L1.L2 events, but the L2 pulse height is not recorded. The same discriminator that controls the pulse height analysis is used to increment the counting rate accumulators corresponding to L1.(NOT L2) and L1.L2 events. 3. Electron Current Detector. The ECD was developed especially for the extremely high fluxes of electrons with energies >3 MeV in the inner Jovian magnetosphere. It consists of a shielded, single solid state detector which operates in current mode at temperatures below -40 degrees (C). Current flow due to formation of electron-hole pairs produced by incident charged particles is linear for electron fluxes up to at least 10**11 electrons/cm**2 sr. Current flow is measured by a logarithmic amplifier which has no significant response to single electron events, so the use of the ECD is restricted to high flux environments. Beryllium shielding absorbs protons and ions below 35 MeV/amu in energy while allowing electrons at energies >= 3.4 MeV to penetrate. The light metallic element Be was chosen to minimize Bremsstrahlung and electron range scattering. The external mount and surface treatment of the ECD cool it to temperatures in the nominal range where the leakage current is 5x(10**(-11)) Ampere. Flux measurements with the ECD have accuracies of approximately a factor two or three, primarily as a result of variations in sensitivity with spectral form and direction of incidence. 4. The fission cell was designed to detect and measure a high-energy proton component in the presence of intense fluxes of high energy electrons. The technique used is to measure the fission fragments resulting from proton- induced fission in the isotope Th-232, since the ratio of cross sections for nucleon-induced fission to electron-induced fission is 10**3 to 10**5, depending on electron energy. In order to measure the fission fragment spectrum, two electrically connected curved silicon surface-barrier detectors surround a 5-mil fission foil of Th-232. The detectors are curved to minimize the possibility of confusing a proton-induced fission event with a high-energy particle having a pathlength long enough to produce a larger signal. The threshold energy of the fission cell, 35 MeV, is determined by the Th-232 coulomb barrier and the minimum amount of 1 gm/cm**2 shielding material. Two counting rates, F1 and F2, are obtained by setting the detector discriminator levels at 30 and 50 MeV, respectively. In this way a ratio F1/F2 is gained which is useful for determination of species or energy spectra of incident particles, the response being significantly different for light and heavy ions. The fission cell was used primarily in the Jovian and Saturnian magnetospheres. B. Data_Channel_Identifiers: ***************************************************************************** Detector Combination ID Code Species Energies Geometry Factor (sqcm-ster.) Pion-10 Pion-11 ------------------------------------------------------------------------------ D1.S.NOT(D2 or D7) 1 P, He 3-10 MeV/amu ~7 ~7 1 CNO 5-20 MeV/amu ~7 ~7 D1.D2.S.NOT(D3 or D7) 2 P, He 11-20 MeV/amu 1.30 1.27 2 C 18-35 MeV/amu 1.30 1.27 2 N 20-40 MeV/amu 1.30 1.27 2 O 22-45 MeV/amu 1.30 1.27 D1.D2.S.D3.NOT(D4 or D7)* 3 P, He 20-24 MeV/emu 1.35 1.27 3 C 35-42 MeV/amu 1.35 1.27 3 N 40-47 MeV/amu 1.35 1.27 3 O 45-52 MeV/amu 1.35 1.27 D1.D2.D4.NOT(D5 or D7) 4 P, He 24-29 MeV/amu 0.388 0.419 4 C 42-50 MeV/amu 0.388 0.419 4 N 47-55 MeV/amu 0.388 0.419 4 O 52-60 MeV/amu 0.388 0.419 4 e- 2- 7 MeV 0.388 0.419 D1.D2.D4.D5.NOT(D6 or D7) 5 P, He 29-67 MeV/amu 0.388 0.419 5 C 50-125 MeV/amu 0.388 0.419 5 N 55-140 MeV/amu 0.388 0.419 5 O 60-185 MeV/amu 0.388 0.419 5 e- 6-28 MeV 0.388 0.419 D1.D2.D4.D5.D6.NOT(D7) 7 P, He >67 MeV/amu ~2 ~2 7 C >125 MeV/amu ~2 ~2 7 N >140 MeV/amu ~2 ~2 7 O >185 MeV/amu ~2 ~2 L1.NOT(L2) P 0.5-1.85 MeV 0.486 0.486 He 0.3-1.82 MeV/amu 0.486 0.486 L1.L2 P 1.85-8.80 MeV 0.486 0.486 He 1.82-50 MeV/amu 0.486 0.486 ------------------------------------------------------------------------------ *Note: This logic is correct for the Pioneer 10 instrument only; for the Pioneer-11 this logic was changed to: D1.D2.S.D3.NOT(D4 or D5 or D6 or D7) Because of the difference in the ID3 logic between the Pioneer 10 and Pioneer 11 instruments, rates and fluxes for this ID should not be combined or added from the two instruments. ****************************************************************************** C. Data_Readout: The CPI instrument readout of high priority rate and pulse height (PHA) information utilizes a four-frame cycle, where 33 bits are allotted to CPI in each main frame word, consisting of 192 data bits. The cycle proceeds as rate 1 word PHA word, rate 2 word, and PHA word, where a rate 1 word includes the counting rates defined by the detector coincidences D1.S.NOT(D2 or D3 or D7) and L1.NOT(L2). A rate 2 word contains the counting rates defined by D1.D2.S.NOT(D3 or D4 or D7) and D1.D2.D4.D5.NOT(D6 or D7). Every other mainframe word is devoted to the pulse-height analysis of a single particle event. Also included in each main frame PHA word is information concerning the event range ID and the octant with respect to the solar direction in which the telescope was pointing at the instant the event was detected. Read out concurrently with the main frame is a science subcommutator word of 6 bits. One science subcom frame requires 64 main frame readouts for completion. Lower priority MT rates as well as the analog and digital information provided by the other three sensors in the instrument package are sequentially read out in this way. Consequently, the subcom information is read out only 1/16 as often as any one of the main frame rates defined above. Data_Set_Parameters: The parameters in this dataset provide information to allow computation of average counting rates and of fluxes of protons, electrons, helium and CNO-group nuclei in selected energy ranges as identified by the pulse height analysis (see the PHINT-tape description, below). /* Note: a 'FORMAT' of 'in' means the item is an ASCII integer */ /* of 'n' characters and should be read with a FORTRAN */ /* FORMAT specification of 'In' -- e.g. 'I6'. Time is */ /* referenced to Spacecraft Event Time */ WORD CONTENTS RANGE FORMAT 01 S/C identification Number 10 or 11 i3 02 10*Seconds of Day at interval start time 0 - 864000 i7 03 Day of Year (Jan. 1 = 1) 0 - 366 i4 04 Year from 1970 2 - 32 i4 05 Coverage (seconds) for Rate #1 : L1N2 0 - 900 i5 06 Counts for Rate #1 : L1N2 0 - 100000 i8 07 Coverage (seconds) for Rate #2 : D1SN2 0 - 900 i5 08 Counts for Rate #2 : D1SN2 0 - 100000 i8 09 Coverage (seconds) for Rate #3 : D12SN3 0 - 900 i5 10 Counts for Rate #3 : D12SN3 0 - 1500 i8 11 Coverage (seconds) for Rate #4 : D1245N6 0 - 900 i5 12 Counts for Rate #4 : D1245N6 0 - 1500 i8 13 Coverage (seconds) for Rate #5 : D2456N7 0 - 900 i5 14 Counts for Rate #5 : D2456N7 0 - 1500 i8 15 Coverage (seconds) for Rate #6 : D12NS 0 - 900 i5 16 Counts for Rate #6 : D12NS 0 - 1500 i8 17 Coverage (seconds) for Rate #7 : L12 0 - 900 i5 18 Counts for Rate #7 : L12 0 - 1500 i8 19 Coverage (seconds) for Fission 1 Rate: 0 - 900 i5 FISS1 20 Counts for Fission 1 Rate : FISS1 0 - 100 i8 21 Coverage (seconds) for Fission 2 Rate: 0 - 900 i5 FISS2 22 Counts for Fission 2 Rate : FISS2 0 - 100 i8 23 Coverage (seconds) for ECD Rate: ECD 0 - 900 i5 24 Counts for ECD Rate: ECD 0 - 100 i8 25 Coverage (seconds) for the subcom rate: 0 - 900 i5 D7 26 Counts for the subcom rate : D7 0 - 1000000 i8 27 Total number of PH events for ID1 0 - 2000 i5 28 Total number of PH events for ID2 0 - 2000 i5 29 Total number of PH events for ID5 0 - 2000 i5 30 Total number of PH events for ID7 + ID13 0 - 2000 i5 31 Total number of PH events for ID13 0 - 2000 i5 32 Counts for PH Box #01: 0 - 1000 i5 ID1 Protons (3 - 10 MeV) 33 Counts for PH Box #02: 0 - 1000 i5 ID1 Helium (3 - 10 MeV/amu) 34 Counts for PH Box #03: 0 - 100 i5 ID1 CNO 35 Counts for PH Box #04: 0 - 1000 i5 ID2 Protons (11 - 20 MeV) 36 Counts for PH Box #05: ID2 Protons (11.00 - 13.25 MeV) 0 - 1000 i5 37 Counts for PH Box #06: ID2 Protons (13.25 - 15.50 MeV) 0 - 1000 i5 38 Counts for PH Box #07: ID2 Protons ((15.50 - 17.75 MeV) 0 - 1000 i5 39 Counts for PH Box #08: ID2 Protons (17.75 - 20.00 MeV) 0 - 1000 i5 40 Counts for PH Box #09: 0 - 100 i5 ID2 Helium (11 - 20 MeV/amu) 41 Counts for PH Box #10: 0 - 1000 i5 ID3 Protons (20 - 24 MeV) 42 Counts for PH Box #11: 0 - 100 i5 ID3 Helium (20 - 24 MeV/amu) 43 Counts for PH Box #12: ID4 Electrons 0 - 100 i5 44 Counts for PH Box #13: 0 - 1000 i5 ID4 Protons (24 - 29 MeV) 45 Counts for PH Box #14: 0 - 10 i5 ID4 Helium (24 - 29 MeV/amu) 46 Counts for PH Box #15: ID4 Z > 2 0 - 100 i5 47 Counts for PH Box #16: ID5 Electrons 0 - 100 i5 48 Counts for PH Box #17: 0 - 100 i5 ID5 Electrons (2 x min. ion.) 49 Counts for PH Box #18: 0 - 1000 i5 ID5 Protons (29 - 67 MeV) 50 Counts for PH Box #19: ID5 Protons (29 - 42 MeV) 0 - 1000 i5 51 Counts for PH Box #20: ID5 Protons (42 - 54 MeV) 0 - 1000 i5 52 Counts for PH Box #21: ID5 Protons (54 - 67 MeV) 0 - 1000 i5 53 Counts for PH Box #22: 0 - 100 i5 ID5 Helium (29 - 67 MeV/amu) 54 Counts for PH Box #23: ID5 Z>2 0 - 100 i5 55 Counts for PH Box #24: ID7 Z>5 0 - 100 i5 56 Counts for PH Box #25: ID9 Electrons 0 - 100 i5 57 Counts for PH Box #26: ID10 Electrons 0 - 100 i5 58 Counts for PH Box #27: 0 - 2000 i5 ID7 + ID13 (> 67 MeV/amu) 59 100*S/C longitude (Heliographic coord.) -18000 - 18000 i7 60 100*S/C latitude (Heliographic coord.) -9000 - 9000 i7 61 100*Radial Distance of s/c from the sun 100 - 8000 i7 62 S/C Telemetry rate (bps) 16 - 2048 i5 63 Effective bit rate (bps) 8 - 2048 i5 64 S/C Spin Rate (rpm x 1000) 4000 - 9000 i5 Data_Set_Quality: Most erroneous data has been removed from the dataset. A few 15-minute data-logical-records (see "Data_Organization", below) contain data which is of dubious quality; these logical-records are flagged by setting the first data-item (item #01, "Spacecraft Identification Number") to the value 00000 (zero). In addition, any logical record for which there was no telemetry coverage has this data item set to zero (see "Data_Organization"); thus, any logical record which has a zero in the first data-item should be ignored -- this check must be made before any other data or time checks are made. Data_Processing_Overview: A. Experimenter Data Records (EDR): The basic experiment data from the CPI is supplied by the Ames Research Center (ARC) in EDR format. Each EDR contains the data from a 24-hour period and contains four physical files. The first of these is a BCD file containing general information about the spacecraft operations and about the ARC processing for this period. The second file is also BCD and contains a record of all commands sent to the spacecraft during the period of the EDR. The third file is in 24-bit binary words and contains the latest 31 observations of celestial latitude, longitude, clock angle of the Sun, and clock angle of Canopus. The fourth file presents the CPI data for the period in physical records consisting of a 24-bit-word binary header (34 words) and then the CPI data in 256 24-bit binary words, as extracted from 128 spacecraft data frames. The CPI Rate-scaler values in the EDR are in log-compressed form as described in the document below. The contents of the UC-CPI EDR are documented in a NASA document, Pioneer Off-line Data Processing System Experimenter Tape Formats October, 1966 Prepared for Ames Research Center, Moffett Field, CA, by Computer Sciences Corporation. and in an internal University of Chicago-LASR document, JUPRO Primary Processing Program for Pioneer 10/11 CPI Data 12/12/72 B. Primary Processing of CPI Data: The basic processing program for the CPI data accepts the EDR-format data files as described above and produces the "Summary Tape" and "CAL/MRO" datasets described below. This processor provides (1) time validation and time conversion from ground-received time to spacecraft-transmitted time, (2) rejection or flagging of invalid data, (3) rejection of null-pulse-height readouts, (4) computation of sectors (look direction) for both counting rates and valid pulse-height analyses. Since these output data products between them contain all the significant data from the EDR, the EDR is typically recycled after the summary tapes are found to be valid, typically after about 1-2 years. Additional programs are provided to produce, from the Summary Tape, two further data products -- the "Pulse-Height" and "Rate" tapes. These products are the ones which have been the basis of the UC-CPI data submission to the NSSDC for all data from 1972 to the present. The format and content of these datasets are well documented in Simpson et al. [1974b] which is available from the Technical Reference File at NSSDC. Brief descriptions of these datasets are given below. C. The Summary Tape: A complete description of the format of the Summary Tape, Rate tape and Pulse Height tape and of every parameter therein is given in Simpson et al [1974b]. The summary tape contains the bulk of the scientific data from the CPI. These tapes are written in binary mode and 24-bit words (see the above document for a description of these "H800" word formats) and the records are 825 words long. The logical-record structure within these physical records is complex; therefore, these summary tapes are not suitable for distribution. The detailed format of the Summary Tape is documented in the JUPRO document referenced above. A brief description of the contents of the summary tape are given below. No Summary-Tape-format data is included in the dataset being documented here. The summary tape record contains all the significant (i.e., non-fill) rate and (i.e., non-zero) PHA data for all the CPI sensors (MT, LET, ECD, and Fission Cell) at the finest available time resolution and also includes: (1) basic spacecraft and instrument support data - S/C mode, format, frame counter, platform and instrument temperatures, DC bus voltages and current, analog calibration values, instrument on/off status, S/C status words, bit- rate and data-quality indicators. (2) timing data given as the UT year, day-of-year, and milli-second-of-day of the first non-fill frame in the record. (3) calculated angle in the spin plane of the axis of the MT (Main Telescope) for MT pulse-height-analyzed values and rates. Each logical record contains the information from one "engineering-subcom sequence" which includes 128 spacecraft minor frames. D. The Calibrate-Data/Memory-Readout-Data (CAL/MRO) Dataset. The CAL/MRO dataset contains any CPI calibrate-mode or S/C-memory-readout data found during the 24-hour data-day contained in the EDR from which the above- described summary-tape data was derived. In addition, files 1-3 of the CAL/MRO tape will contain copies of the first three files of the EDR as described in paragraph (A) above. If any calibrate-mode or MRO data is found, the fourth file of the CAL/MRO tape contains this data in the same format as the data recorded in a summary- tape logical records as described in paragraph (C) above. E. The Pulse-Height Tape A logical pulse-height record contains all the valid, non-zero pulse-height- analyzed (PHA) data from the MT and LET for a 15-minute period. The logical record (LR) is made up of at least two physical records, (1) header-record (HR) containing - spacecraft-status and instrument-status descriptors - beginning time of the LR in UT - bookkeeping and attitude parameters - "livetime" for the MT during the LR - count of valid MT events - number of filled LET and MT events during the LR - a selection of averaged counting rates correlative with PHA's - livetimes for the correlative counting rates These HR records are expressed in 60, 48-bit floating point (Harris H-800) words. (2) at least one physical record (may be more, depending on the number of analyzed events during the 15-minute period) which contains the PHA values (counts) for each non-zero MT (D1, D2, and D5) and LET (L1) detector, together with range of the analyzed particle through the telescope and the sector (octant of S/C rotation) in which the MT event was detected. These PHA records are expressed in 24-bit integer form. F. The Rate Tape This tape is written in a mixture of 24-bit integer and 48-bit floating-point word (H800) formats. All of the valid, non-fill, rate-scaler values from all CPI detectors are averaged over an rigid five-minute intervals and recorded in this dataset, expressed as average counts/second and associated seconds-of- coverage. For the MT, sectored (octant) rates as well as omnidirectional rates are given; sectoring is to be ignored if the S/C bit rate falls below about 256 bps. Supporting information included in the format is: - beginning/end times of the accumulation interval - S/C status (spin rate, etc.) G. Secondary Processing of CPI Data The secondary processing scheme uses as input the Pulse-Height and Rate tapes described above to determine counting rates and fluxes of various cosmic ray species. The programs involved (1) eliminate bad quality data 2) remove single 5-minute 'spike' events (3) accumulate the good data over fixed time intervals and (4) average over all sectored information. Because the individual time and sector information for each event is lost in the accumulation procedure the Pulse-Height and Rate tapes will continue to be submitted to the NSSDC in case special analysis is desired. H. PHINT-Tape Datasets This is the dataset which is included in the archive in this volume. The PHINT tape (Pulse-Height INTegrated tape) contains all the information necessary to get a basic set of counting rates and fluxes of cosmic rays for various species in selected energy ranges measured with the CPI. The tape is created by processing Pulse-Height tapes and Rate tapes (see E and F above). The standard PHINT tape computes counts during rigid 15-minute intervals in Universal Time at the spacecraft. All 15-minute intervals will be included in the PHINT tape, with times of fill represented by records in which the 1st word (s/c ID number) set to zero. All records should be checked to see if the 1st word is zero before any averaging is done with that record. The PHINT tape has 64 ASCII data-items comprising 357 characters in the format /* ? */ (I3,I7,2I4,11(I5,I8),32I5,3I7,3I5) in each logical (15-minute) record. /* ? */ Housekeeping information and two types of data are stored in the PHINT tape. (1) The housekeeping information includes the spacecraft identifier, the start time for each accumulation interval and spacecraft operation information, the telemetry bit rate, spin rate, radial distance from the Sun, heliographic latitude and longitude is also included. (2) Twenty-seven 'boxes' are defined. Each 'box' contains the total number (counts) in the time interval of a specific charged particle species in a specific energy range. Every non-zero, good Pulse-Height event is analyzed to determine its energy and charge, and then added to the appropriate 'box'. No consistency check is made for the charge determination. Thus during periods of high solar activity many 'boxes' may contain significant numbers of background counts, due to pulse pileup, electronic noise or nuclear interactions occurring in the various detectors. There is also included the total number of pulse-height events in 5 ID's, which can be used as normalization in order to determine fluxes. N.B. There was radiation damage to some of the Pioneer 10 detectors during the passage through the Jovian magnetosphere. The damage has resulted in a slowly varying change in the calculated channel for a given energy deposit in the detectors, most especially D1 and D2. This variation has been corrected for in the 'boxes' on the PHINT tapes. (3) In addition to the 'boxes', eleven important, non-pulse-height analyzed counting rates (counts) are computed. Along with each set of counts is the associated livetime (seconds). With this information counting rates can be calculated. Data_Usage: A. Non-Pulse-Height analyzed rates: The eleven non-pulse-height analyzed counts and coverages can be used to make counting rates for any desired time interval. The user should accumulate the counts and coverages for the desired averaging period, then calculate the rate as: = Sum( counts ) / Sum( coverage ) N.B. To avoid biasing, sums of counts and coverage should be kept for the entire averaging interval. For example, if you wish to compute 24-hour fluxes, do not calculate fluxes for 1 hour periods and then average the 24 1- hour periods, but instead use the PHINT tape to compute true 24-hour sums of both counts and coverage before calculating a counting rate. B. Pulse-Height analyzed rates and fluxes from the 27 'boxes': The user may choose from three possible normalization methods for calculating counting rates for the 27 'boxes' of cosmic rays. If a true flux (particles/cm^2 s sr MeV/n) is desired, you should divide the counting rate by the geometrical factor and the energy interval. (1) Pseudo-count method (pcm) This is the recommended method for calculating counting rates and fluxes. It must be used for accurate values when the counting rates are so low that few or no events are accumulated during a 15- minute interval. It is less accurate during times of high, variable fluxes, but is never grossly incorrect. When the pcm normalization is used, the number of box counts which would have been observed if all incident particles were analyzed is estimated for each 15-minute PHINT tape interval, and these 'pseudo-counts' are summed for the entire averaging period. The pseudo-count total is divided by the appropriate rate coverage total to determine the counting rate. For each 15-minute interval read the four values bxcnt, rtcnt, idcnt and rtcvg from the PHINT tape and calculate the value pcnt as: pcnt = bxcnt * rtcnt / idcnt where bxcnt = number of counts in a matrix 'box' rtcnt = number of counts in the rate scalar associated with the normalizing ID idcnt = number of counts in the normalizing ID rtcvg = seconds of coverage for the rate scalar associated with the normalizing ID pcnt = number of pseudo-counts There are two special cases, in the computation of pcnt, to be considered: (a) If idcnt<>0 and rtcnt=0 for a 15-minute interval, that interval should not used in the computation for this box, since there is not enough information to know what to do. (b) If both idcnt = 0 and rtcnt = 0, you should assume that all events are analyzed. However, since the Pioneer instruments cannot analyze events while a Pulse-Height frame is being read out, there is never 100% analysis. The following table gives the fractional live-times: fractional livetime for fractional livetime for main telescope low energy telescope -------------------------- --------------------------- 0.9141 0.9995 Then if f = fractional livetime, the pseudo-count is defined as: pcnt = bxcnt/f At the end of the averaging interval the mean flux is calculated as follows: = Sum( pcnt ) / Sum( rtcvg ) The University of Chicago has a recommended set of normalizations for each of the 27 'boxes'. The reason for the difference in normalization between Pioneer 10 and Pioneer 11 is that the D4 detector failed on Pioneer 11 in mid- 1980 and no ID5 Pulse-Height events or D1245N6 rate events have been recorded since then. For Pioneer 10: Boxes #01 (ID1 H), #02 (ID1 He), #03 (ID1 CNO), #24 (ID7 Z>5), #25 (ID9 e-), #26 (ID10 e-), and #27 (ID7+ID13 >67MeV/AMU) : use the Pulse-Height #1, ID1 to normalize and use the associated rate #2, D1SN2. All other boxes (#04-#23) : use the Pulse-Height #3, ID5 to normalize and use the associated rate #4, D1245N6. For Pioneer 11: Boxes #01 (ID1 H), #02 (ID1 He), #03 (ID1 CNO), #24 (ID7 Z>5), #25 (ID9 e-), #26 (ID10 e-), and #27 (ID7+ID13 >67MeV/AMU) : use the Pulse-Height #1, ID1 to normalize and use the associated rate #2, D1SN2. All other boxes (#04-#23) : use the Pulse-Height #2, ID2 to normalize and use the associated rate #3, D12SN3. (2) Old method (om) This is the old standard method of normalization. The bxcnts, rtcnts, idcnts, and rtcvgs are summed for the entire averaging interval. Then: Sum( bxcnt ) * Sum( rtcnt ) = ---------------------------------- Sum( idcnt ) * Sum( rtcvg ) If less than 100% of the events are being pulse height analyzed, this method breaks down when the normalizing rate varies significantly during an averaging interval. Thus it works poorly during flare periods, when large transients, such as shocks, pass the spacecraft, and near planetary encounter periods. (3) Pulse-Height-Livetime method (phlt). This method sums bxcnts and phlts for the whole averaging interval. The pulse height livetime for each ID is calculated by dividing the ID counts for a sub-interval by the value of the corresponding rate averaged over that sub-interval. That is, the counters: idcnt, rtcnt, and rtcvg are accumulated during an interval and then phlt = idcnt * rtcvg / rtcnt (see pcm method above for the recommended normalizing ID and associated rate). The counts in a 'box' and the phlts for the sub-intervals are summed to get a phlt for the entire averaging interval. The average flux is calculated as: = Sum( bxcnt ) / Sum( phlt ) This method breaks down when the normalizing rate is so low that few or no counts are accumulated during a 15-minute interval. Data_Organization: A CPI PHINT-tape logical record contains the data (with content and datum-size as specified in the "Data_Set_Parameters" section above and, in the "FORMAT.SFD" file, in the "Record_Syntax" section) for a 15-minute period of time synchronized with hour boundaries. It has a size of 357 ASCII characters (bytes). A physical tape record will consist of a concatenation of ?? logical records, have a size of ??,??? bytes and contain the data from one day. A year of CPI-PHINT data consists of either 365 or 366 such physical records (a total of 12,158,880???? or 12,192,192???? bytes). A year of data will be contained in two or more separate data files, each containing nor more than six months of data. /* ??please review check numbers above??*/ In the case of missing data: (1) if no coverage-time is available for any 15-minute logical record or series of logical records, such logical records have every one of the 64 data- items in them set to zero values; this will make the "Spacecraft Identification Number" be zero and the logical-record can be ignored by an initial check on that item (see also, "Data_Set_Quality" above). (2) if no coverage was obtained for an entire day, the physical record for that day will exist but will consist of ?? zero-logical-records as defined above. This is done to preserve the overall structure so that (for example) FORTRAN 'READs' based on multiple-day FORMAT specifications are easily possible. /* check ?? number above */ File_Class_Relationships: N/A Lit_References: Simpson, J. A., T. S. Bastian, D. L. Chenette, R. B. McKibben, and K. R. Pyle, The trapped radiations of Saturn and their absorption by satellites and rings, J. Geophys. Res., 85, 5731, 1980. Simpson, J. A., D. C. Hamliton, R. B. McKibben, A. Mogro-Campero, K. R. Pyle, and A. J. Tuzzolino, The protons and electrons trapped in the Jovian dipole magnetic field and their interaction with Io, J. Geophys. Res., 79, 3522, 1974a. Simpson, J. A., G. A. Lentz, R. B. McKibben, J. J. O'Gallagher, W. Schroeder, and A. J. Tuzzolino, Preliminary documentation for the University of Chicago charged particle instrument from the Pioneer 10/11 spacecraft, NSSDC Tech. Ref. File B21970, Goddard Space Flight Center, Greenbelt, MD, 1974b. CCSD$$MARKERMRK**002CCSD3KS00002MRK**003 Vol_Time_Coverage: 1973-04-05 to 1983-12-31 /* | */ /* | A second volume will cover (for Pioneer 11) 1984-01-01 to 1992-12-31 And subsequent volumes will contain 1 year of data: 1993-01-01 to 1993-12-31 1994-01-01 to 1994-12-31 etc. ......... */ File_Naming_Convention: CPI files are named according to the start time of the data contained in the file, using the form CPI_PXX_YYH.DAT where: PXX can be either P10 or P11 YY stands for the last two digits of the year H can be A, meaning "first half of the calendar year, i.e., January/01 through June/30" or B, meaning "second half of the calendar year, i.e., July/01 through December/31." Note that files on the current data volume are referenced below by file sequence number, since there are no file labels on the tape. These sequence numbers are then mapped to the actual file name in the "REFERENCE=" keywords. File_Time_Coverage: /* | */ CPI_P11_73A.DAT 73/04/05 thru 73/06/30 CPI_P11_73B.DAT 73/07/01 thru 73/12/31 . (continuation of series) . . CPI_P11_83B.DAT 83/07/01 thru 83/12/31 /* | Note: other volumes will contain the following: CPI_P11_84A.DAT 84/01/01 thru 84/06/30 . through... . CPI_P11_92B.DAT 92/07/01 thru 92/12/31 with annual volumes thereafter. */ CCSD$$MARKERMRK**003NSSD3RF0014000000001 REFERENCETYPE = $SEQUENCE; LABEL=ATTACHED; REFERENCE = "$2 = FORMAT.SFD, $5 = 2"; LABEL = NSSD3IF0013200000001; REFERENCE = "$2 = CPI_P11_72A.DAT, $5 = 3"; REFERENCE = "$2 = CPI_P11_72B.DAT, $5 = 4"; REFERENCE = "$2 = CPI_P11_73A.DAT, $5 = 5"; REFERENCE = "$2 = CPI_P11_73B.DAT, $5 = 6"; REFERENCE = "$2 = CPI_P11_74A.DAT, $5 = 7"; REFERENCE = "$2 = CPI_P11_74B.DAT, $5 = 8"; REFERENCE = "$2 = CPI_P11_75A.DAT, $5 = 9"; REFERENCE = "$2 = CPI_P11_75B.DAT, $5 = 10"; REFERENCE = "$2 = CPI_P11_76A.DAT, $5 = 11"; REFERENCE = "$2 = CPI_P11_76B.DAT, $5 = 12"; REFERENCE = "$2 = CPI_P11_77A.DAT, $5 = 13"; REFERENCE = "$2 = CPI_P11_77B.DAT, $5 = 14"; REFERENCE = "$2 = CPI_P11_78A.DAT, $5 = 15"; REFERENCE = "$2 = CPI_P11_78B.DAT, $5 = 16"; REFERENCE = "$2 = CPI_P11_79A.DAT, $5 = 17"; REFERENCE = "$2 = CPI_P11_79B.DAT, $5 = 18"; REFERENCE = "$2 = CPI_P11_80A.DAT, $5 = 19"; REFERENCE = "$2 = CPI_P11_80B.DAT, $5 = 20"; REFERENCE = "$2 = CPI_P11_81A.DAT, $5 = 21"; REFERENCE = "$2 = CPI_P11_81B.DAT, $5 = 22"; REFERENCE = "$2 = CPI_P11_82A.DAT, $5 = 23"; REFERENCE = "$2 = CPI_P11_82B.DAT, $5 = 24"; REFERENCE = "$2 = CPI_P11_83A.DAT, $5 = 25"; REFERENCE = "$2 = CPI_P11_83B.DAT, $5 = 26"; /* */ CCSD3FF0000500000001CCSD3CS00004MRK**001 ADIDNAME=NSSD0132; CCSD$$MARKERMRK**001CCSD3KS00002MRK**002 Subm_Name: Gordon A. Lentz Subm_Addr: Gordon A. Lentz University of Chicago Enrico Fermi Institute Laboratory for Astrophysics and Space Research 933 E. 56th Street Chicago, IL 60637 Telephone: (312) 702-7836 E-Mail: (NSI/DECnet) LASR::LENTZ : (Internet) lentz@odysseus.uchicago.edu Subm_Date: TBD /* e.g.: 1991-01-05 | */ Title: Format for Pioneer 11 CPI Cruise Data Archive Data Set Descr: Format description of the Pioneer 11 Charged Particle Instrument's cruise phase archive data set, April, 1973 through December, 1992 Rel_Date: 1991-01-05 CCSD$$MARKERMRK**002CCSD3DF0000200000001 File_Class_Name: UC CPI Interplanetary Cruise ASCII Archive Record_Type_Name: Fifteen-minute PHINT tape Algorithms: See VOLDESC.SFD file, Data_Usage section. All algorithms used in the interpretation of the CPI data are given in detail there. File_Class_Syntax: All records in the UC CPI interplanetary cruise ASCII archive files are of the same type, size, and format. File_Class_Field_Relationships: N/A File_Class_Misc: See Record and Field specifications. Record_Name: Fifteen-minute PHINT tape records Record_Structure: All data records are of the same length. Record_Length: ??,??? ASCII characters or bytes per physical record. /* ? */ Each physical record contains ?? logical records of /* ? */ length 357 bytes. /* ? */ Record_Field_Names: SCID,ISTIM,DOY,YEAR70,TL1NL2,CL1NL2,TD1SN2,CD1SN2,TD12SN3,CD12SN3,TD1245N6, CD1245N6,TD2456N7,CD2456N7,TD12NS,CD12NS,TL1L2,CL1L2,TFISS1,CFISS1,TFISS2, CFISS2,TECD,CECD,TD7,CD7,NPHID1,NPHID2,NPHID5,NPHID713,NPHID13,NID1P,NID1HE, NID1CNO,NID2P1,NID2P2,NID2P3,NID2P4,NID2P5,NID2HE,NID3P,NID3HE,NID4E,NID4P, NID4HE,NID4ZG2,NID5E1,NID5E2,NID5P1,NID5P2,NID5P3,NID5P4,NID5HE,NID5ZG2, NID7ZG5,NID9E,NID10E,NID7+13,HEGLONG,HEGLAT,HEGRAD,TELBRATE,EFFBRATE,SPINRATE FORMAT (I3,I7,2I4,11(I5,I8),32I5,3I7,3I5) /* ? */ Record_Syntax: (See the note preceding the "Data_Set_Parameters" Table.) WORD MNEMONIC CONTENTS RANGE FORMAT 01 SCID S/C identification Number 10 or 11 i3 02 ISTIM 10*Seconds of Day at interval start time 0 - 864000 i7 03 DOY Day of Year (Jan. 1 = 1) 0 - 366 i4 04 YEAR70 Year from 1970 2 - 32 i4 05 TL1NL2 Coverage (seconds) for Rate #1 : L1N2 0 - 900 i5 06 CL1NL2 Counts for Rate #1 : L1N2 0 - 100000 i8 07 TD1SN2 Coverage (seconds) for Rate #2 : D1SN2 0 - 900 i5 08 CD1SN2 Counts for Rate #2 : D1SN2 0 - 100000 i8 09 TD12SN3 Coverage (seconds) for Rate #3 : D12SN3 0 - 900 i5 10 CD12SN3 Counts for Rate #3 : D12SN3 0 - 1500 i8 11 TD1245N6 Coverage (seconds) for Rate #4 : D1245N6 0 - 900 i5 12 CD1245N6 Counts for Rate #4 : D1245N6 0 - 1500 i8 13 TD2456N7 Coverage (seconds) for Rate #5 : D2456N7 0 - 900 i5 14 CD2456N7 Counts for Rate #5 : D2456N7 0 - 1500 i8 15 TD12NS Coverage (seconds) for Rate #6 : D12NS 0 - 900 i5 16 CD12NS Counts for Rate #6 : D12NS 0 - 1500 i8 17 TL1L2 Coverage (seconds) for Rate #7 : L12 0 - 900 i5 18 CL1L2 Counts for Rate #7 : L12 0 - 1500 i8 19 TFISS1 Coverage (seconds) for Fission 1 Rate: 0 - 900 i5 FISS1 20 CFISS1 Counts for Fission 1 Rate : FISS1 0 - 100 i8 21 TFISS2 Coverage (seconds) for Fission 2 Rate: 0 - 900 i5 FISS2 22 CFISS2 Counts for Fission 2 Rate : FISS2 0 - 100 i8 23 TECD Coverage (seconds) for ECD Rate: ECD 0 - 900 i5 24 CECD Counts for ECD Rate: ECD 0 - 100 i8 25 TD7 Coverage (seconds) for the subcom rate: 0 - 900 i5 D7 26 CD7 Counts for the subcom rate : D7 0 - 1000000 i8 27 NPHID1 Total number of PH events for ID1 0 - 2000 i5 28 NPHID2 Total number of PH events for ID2 0 - 2000 i5 29 NPHID5 Total number of PH events for ID5 0 - 2000 i5 30 NPHID713 Total number of PH events for ID7 + ID13 0 - 2000 i5 31 NPHID13 Total number of PH events for ID13 0 - 2000 i5 32 NID1P Counts for PH Box #01: 0 - 1000 i5 D1 Protons (3 - 10 MeV) 33 NID1HE Counts for PH Box #02: 0 - 1000 i5 ID1 Helium (3 - 10 MeV/amu) 34 NID1CNO Counts for PH Box #03: 0 - 100 i5 ID1 CNO 35 NID2P1 Counts for PH Box #04: 0 - 1000 i5 ID2 Protons (11 - 20 MeV) 36 NID2P2 Counts for PH Box #05: 0 - 1000 i5 ID2 Protons (11.00 - 13.25 MeV) 37 NID2P3 Counts for PH Box #06: 0 - 1000 i5 ID2 Protons (13.25 - 15.50 MeV) 38 NID2P4 Counts for PH Box #07: 0 - 1000 i5 ID2 Protons (15.50 - 17.75 MeV) 39 NID2P5 Counts for PH Box #08: 0 - 1000 i5 ID2 Protons (17.75 - 20.00 MeV) 40 NID2HE Counts for PH Box #09: 0 - 100 i5 ID2 Helium (11 - 20 MeV/amu) 41 NID3P Counts for PH Box #10: 0 - 1000 i5 ID3 Protons (20 - 24 MeV) 42 NID3HE Counts for PH Box #11: 0 - 100 i5 ID3 Helium (20 - 24 MeV/amu) 43 NID4E Counts for PH Box #12: ID4 Electrons 0 - 100 i5 44 NID4P Counts for PH Box #13: 0 - 1000 i5 ID4 Protons (24 - 29 MeV) 45 NID4HE Counts for PH Box #14: 0 - 10 i5 ID4 Helium (24 - 29 MeV/amu) 46 NID4ZG2 Counts for PH Box #15: ID4 Z > 2 0 - 100 i5 47 NID5E1 Counts for PH Box #16: ID5 Electrons 0 - 100 i5 48 NID5E2 Counts for PH Box #17: 0 - 100 i5 ID5 Electrons (2 x min. ion.) 49 NID5P1 Counts for PH Box #18: 0 - 1000 i5 ID5 Protons (29 - 67 MeV) 50 NID5P2 Counts for PH Box #19: 0 - 1000 i5 ID5 Protons (29 - 42 MeV) 51 NID5P3 Counts for PH Box #20: 0 - 1000 i5 ID5 Protons (42 - 54 MeV) 52 NID5P4 Counts for PH Box #21: 0 - 1000 i5 ID5 Protons (54 - 67 MeV) 53 NID5HE Counts for PH Box #22: 0 - 100 i5 ID5 Helium (29 - 67 MeV/amu) 54 NID5ZG2 Counts for PH Box #23: ID5 Z>2 0 - 100 i5 55 NID7ZG5 Counts for PH Box #24: ID7 Z>5 0 - 100 i5 56 NID9E Counts for PH Box #25: ID9 Electrons 0 - 100 i5 57 NID10E Counts for PH Box #26: ID10 Electrons 0 - 100 i5 58 NID7+13 Counts for PH Box #27: 0 - 2000 i5 ID7 + ID13 (> 67 MeV/amu) 59 HEGLONG 100*S/C longitude (Heliographic coord.) -18000 - 18000 i7 60 HEGLAT 100*S/C latitude (Heliographic coord.) -9000 - 9000 i7 61 HEGRAD 100*Radial Distance of s/c from the sun 100 - 8000 i7 62 TELBRATE S/C Telemetry rate (bps) 16 - 2048 i5 63 EFFBRATE Effective bit rate (bps) 8 - 2048 i5 64 SPINRATE S/C Spin Rate (rpm x 1000) 4000 - 9000 i5 Field_Name: S/C identification number Field_Mnemonic: SCID Field_Units: ASCII characters Field_Resolution: N/A Field_Range: 10 - 11 Field_Description: S/C identification number (10= P10, 11= P11) Field_Representation: 3 ASCII CHARACTERS (I3) Field_Name: Start time for 15-min interval Field_Mnemonic: ISTIM Field_Units: 10*Seconds of Day Field_Resolution: N/A Field_Range: 0 - 864000 Field_Description: 10*Seconds of Day at interval start time Field_Representation: 7 ASCII characters (I7) Field_Name: Day of Year Field_Mnemonic: DOY Field_Units: Day of year Field_Resolution: 1 day Field_Range: 1-366 Field_Description: Day of Year (Jan. 1 = 1) Field_Representation: 4 ASCII characters (I4) Field_Name: Years from 1970 Field_Mnemonic: YEAR70 Field_Units: year Field_Resolution: 1 year Field_Range: 2-32 Field_Description: Year from 1970 (2 = year 1972) Field_Representation: 4 ASCII characters (I4) Field_Name: L1NL2 time coverage Field_Mnemonic: TL1NL2 Field_Units: seconds Field_Resolution: 1 Field_Range: 0-900 Field_Description: Coverage (seconds) for Rate #1 : L1NL2 Field_Representation: 5 ASCII characters (I5) Field_Name: L1NL2 counts Field_Mnemonic: CL1NL2 Field_Units: counts Field_Resolution: 1 Field_Range: 0-100000 Field_Description: Counts for Rate #1: L1NL2 Field_Representation: 8 ASCII characters (I8) Field_Name: D1SN2 Time Coverage Field_Mnemonic: TD1SN2 Field_Units: seconds Field_Resolution: 1 Field_Range: 0-900 Field_Description: Coverage for Rate #2: D1SN2 Field_Representation: 5 ASCII characters (I5) Field_Name: D1SN2 Counts Field_Mnemonic: CD1SN2 Field_Units: counts Field_Resolution: 1 Field_Range: 0-100000 Field_Description: Counts for Rate #2: D1SN2 Field_Representation: 8 ASCII characters (I8) Field_Name: D12SN3 Time Coverage Field_Mnemonic: TD12SN3 Field_Units: seconds Field_Resolution: 1 Field_Range: 0-900 Field_Description: Coverage for Rate #3: D12SN3 Field_Representation: 5 ASCII characters (I5) Field_Name: D12SN3 Counts Field_Mnemonic: CD12SN3 Field_Units: counts Field_Resolution: 1 Field_Range: 0-1500 Field_Description: Counts for Rate #3 Field_Representation: 8 ASCII characters (I8) Field_Name: D1245N6 Coverage Field_Mnemonic: TD1245N6 Field_Units: seconds Field_Resolution: 1 Field_Range: 0-900 Field_Description: Coverage for Rate #4: D1245N6 Field_Representation: 5 ASCII characters (I5) Field_Name: D1245N6 Counts Field_Mnemonic: CD1245N6 Field_Units: counts Field_Resolution: 1 Field_Range: 0-1500 Field_Description: Counts for Rate #4: D1245N6 Field_Representation: 8 ASCII characters (I8) Field_Name: D2456N7 Coverage Field_Mnemonic: TD2456N7 Field_Units: seconds Field_Resolution: 1 Field_Range: 0-900 Field_Description: Coverage for Rate #5: D2456N7 Field_Representation: 5 ASCII characters (I5) Field_Name: D2456N7 Counts Field_Mnemonic: CD2456N7 Field_Units: counts Field_Resolution: 1 Field_Range: 0-1500 Field_Description: Counts for Rate #5: D2456N7 Field_Representation: 8 ASCII characters (I8) Field_Name: D12NS Coverage Field_Mnemonic: TD12NS Field_Units: seconds Field_Resolution: 1 Field_Range: 0-900 Field_Description: Coverage for Rate #6: D12NS Field_Representation: 5 ASCII characters (I5) Field_Name: D12NS Counts Field_Mnemonic: CD12NS Field_Units: counts Field_Resolution: 1 Field_Range: 0-1500 Field_Description: Counts for Rate #6: D12NS Field_Representation: 8 ASCII characters (I8) Field_Name: L1L2 Coverage Field_Mnemonic: TL1L2 Field_Units: seconds Field_Resolution: 1 Field_Range: 0-900 Field_Description: Coverage for Rate #7: L1L2 Field_Representation: 5 ASCII characters (I5) Field_Name: L1L2 Counts Field_Mnemonic: CL1L2 Field_Units: counts Field_Resolution: 1 Field_Range: 0-1500 Field_Description: Counts for Rate #7: L1L2 Field_Representation: 8 ASCII characters (I8) Field_Name: Fission 1 Coverage Field_Mnemonic: TFISS1 Field_Units: seconds Field_Resolution: 1 Field_Range: 0-900 Field_Description: Coverage for Fission 1 Rate: FISS1 Field_Representation: 5 ASCII characters (I5) Field_Name: Fission 1 Counts Field_Mnemonic: CFISS1 Field_Units: counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: Counts for Fission 1 Rate: FISS1 Field_Representation: 8 ASCII characters (I8) Field_Name: Fission 2 Coverage Field_Mnemonic: TFISS2 Field_Units: seconds Field_Resolution: 1 Field_Range: 0-900 Field_Description: Coverage for Fission 2 Rate: FISS2 Field_Representation: 5 ASCII characters (I5) Field_Name: Fission 2 Counts Field_Mnemonic: CFISS2 Field_Units: counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: Counts for Fission 2 Rate: FISS2 Field_Representation: 8 ASCII characters (I8) Field_Name: Electron Current Detector Rate (ECD) Coverage Field_Mnemonic: TECD Field_Units: seconds Field_Resolution: 1 Field_Range: 0-900 Field_Description: Coverage for ECD Rate: ECD Field_Representation: 5 ASCII characters (I5) Field_Name: Electron Current Detector Rate (ECD) Counts Field_Mnemonic: CECD Field_Units: counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: Counts for ECD Rate: ECD Field_Representation: 8 ASCII characters (I8) Field_Name: D7 Coverage Field_Mnemonic: TD7 Field_Units: seconds Field_Resolution: 1 Field_Range: 0-900 Field_Description: Coverage for D7 subcom rate Field_Representation: 5 ASCII characters (I5) Field_Name: D7 Counts Field_Mnemonic: CD7 Field_Units: counts Field_Resolution: 1 Field_Range: 0-1000000 Field_Description: Counts for the D7 subcom rate Field_Representation: 8 ASCII characters (I8) Field_Name: ID1 PH Events Field_Mnemonic: NPHID1 Field_Units: events Field_Resolution: 1 Field_Range: 0-2000 Field_Description: Total number of PH events for ID1 Field_Representation: 5 ASCII characters (I5) Field_Name: ID2 PH events Field_Mnemonic: NPHID2 Field_Units: events Field_Resolution: 1 Field_Range: 0-2000 Field_Description: Total number of PH events for ID2 Field_Representation: 5 ASCII characters (I5) Field_Name: ID5 PH events Field_Mnemonic: NPHID5 Field_Units: events Field_Resolution: 1 Field_Range: 0-2000 Field_Description: Total number of PH events for ID5 Field_Representation: 5 ASCII characters (I5) Field_Name: ID7+ID13 PH Events Field_Mnemonic: NPHID713 Field_Units: events Field_Resolution: 1 Field_Range: 0-2000 Field_Description: Total number of PH events for ID7+ID13 Field_Representation: 5 ASCII characters (I5) Field_Name: ID13 PH Events Field_Mnemonic: NPHID13 Field_Units: events Field_Resolution: 1 Field_Range: 0-2000 Field_Description: Total PH Events for ID13 Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 1 Counts Field_Mnemonic: NID1P Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID1 Protons (3-10 MeV) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 2 Counts Field_Mnemonic: NID1HE Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID1 Helium (3 - 10 MeV/amu) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 3 Counts Field_Mnemonic: NID1CNO Field_Units: Counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: ID1 CNO Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 4 Counts Field_Mnemonic: NID2P1 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID2 Protons (11 - 20 MeV) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 5 Counts Field_Mnemonic: NID2P2 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID2 Protons (11.00-13.25 MeV) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 6 Counts Field_Mnemonic: NID2P3 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID2 Protons (13.25-15.50 MeV) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 7 Counts Field_Mnemonic: NID2P4 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID2 Protons (15.50-17.75 MeV) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 8 Counts Field_Mnemonic: NID2P5 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID2 Protons (17.75-20.00 MeV) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 9 Counts Field_Mnemonic: NID2HE Field_Units: Counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: ID2 Helium (11 - 20 MeV/amu) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 10 Counts Field_Mnemonic: NID3P Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID3 Protons (20 - 24 MeV) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 11 Counts Field_Mnemonic: NID3HE Field_Units: Counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: ID3 Helium (20 - 24 MeV/amu) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 12 Counts Field_Mnemonic: NID4E Field_Units: Counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: ID4 Electrons Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 13 Counts Field_Mnemonic: NID4P Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID4 Protons (24 - 29 MeV) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 14 Counts Field_Mnemonic: NID4HE Field_Units: Counts Field_Resolution: 1 Field_Range: 0-10 Field_Description: ID4 Helium (24 - 29 MeV/amu) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 15 Counts Field_Mnemonic: NID4ZG2 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: ID4 Z > 2 Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 16 Counts Field_Mnemonic: NID5E1 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: ID5 Electrons Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 17 Counts Field_Mnemonic: NID5E2 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: ID5 Electrons (2 x Min.Ion.) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 18 Counts Field_Mnemonic: NID5P1 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID5 Protons (29 - 67 MeV) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 19 Counts Field_Mnemonic: NID5P2 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID5 Protons (29 - 42 MeV) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 20 Counts Field_Mnemonic: NID5P3 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID5 Protons (42 - 54 MeV) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 21 Counts Field_Mnemonic: NID5P4 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-1000 Field_Description: ID5 Protons (54 - 67 MeV) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 22 Counts Field_Mnemonic: NID5HE Field_Units: Counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: ID5 Helium (29 - 67 MeV/amu) Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 23 Counts Field_Mnemonic: NID5ZG2 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: ID5 Z > 2 Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 24 Counts Field_Mnemonic: NID7ZG5 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: ID7 Z > 5 Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 25 Counts Field_Mnemonic: NID9E Field_Units: Counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: ID9 Electrons Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 26 Counts Field_Mnemonic: NID10E Field_Units: Counts Field_Resolution: 1 Field_Range: 0-100 Field_Description: ID10 Electrons Field_Representation: 5 ASCII characters (I5) Field_Name: PH Box 27 Counts Field_Mnemonic: NID7+13 Field_Units: Counts Field_Resolution: 1 Field_Range: 0-2000 Field_Description: ID7 + ID13 (>67 MeV/amu) Field_Representation: 5 ASCII characters (I5) Field_Name:S/C Heliographic Longitude Field_Mnemonic: HEGLONG Field_Units: 100*degrees Field_Resolution: .01 degrees Field_Range:-18,000 -- 18,000 Field_Description: Heliographic Longitude of S/C in 0.01-degrees Field_Representation: 7 ASCII Characters (I7) Field_Name: S/C Heliographic Latitude Field_Mnemonic: HEGLAT Field_Units: 100*degrees Field_Resolution: 0.01 degrees Field_Range: -9,000 -- 9,000 Field_Description: Heliographic Latitude of S/C in 0.01-degree Field_Representation: 7 ASCII Characters (I7) Field_Name: Radial Distance of S/C from Sun Field_Mnemonic: HEGRAD Field_Units: 100*AU Field_Resolution: .01AU Field_Range: 100 -- 8000 Field_Description: Radial distance of the Spacecraft from the Sun in 0.01AU Field_Representation: 7 ASCII Characters (I7) Field_Name: S/C telemetry rate Field_Mnemonic: TELBRATE Field_Units: bits-per-second Field_Resolution: 1 bps Field_Range: 16-2048 Field_Description: S/C Telemetry rate (bps) Field_Representation: 5 ASCII characters (I5) Field_Name: Effective bit rate Field_Mnemonic: EFFBRATE Field_Units: bits-per-second Field_Resolution: 1 bps Field_Range: 8-2048 Field_Description: Effective bit rate Field_Representation: 5 ASCII characters (I5) Field_Name: S/C spin rate Field_Mnemonic: SPINRATE Field_Units: rpm x 1000 Field_Resolution: 1 Field_Range: 4000-9000 Field_Description: S/C Spin Rate Field_Representation: 5 ASCII characters (I5) /* */