2.0.1 spase://nssdc/numericalData/SPMS-00147 ISEE 1 Data Pool Set 2008-02-21T00:00:00 This quick-look data pool data set contains selected physical parameters computed centrally for each instrument at resolutions between one and five minutes, using quick-look, PI-provided algorithms. It was created in binary IBM 360 representation with unblocked, 3240-byte records. The first record of each file is a data pool file label containing satellite ID number; year, day of year, and seconds of day for the start and end of file; spacecraft clock; telemetry group number; minimum and maximum value of spin period found in this file; shadow times; and bit rate. The label record is followed by a number of data records containing day of year and seconds of day; s/c clock; bit rate; housekeeping and engineering items; spin period average; satellite position vector in GSE coordinates; and outputs of the investigators' quick-look data-processing algorithms for selected parameters from ten of the onboard experiments. The fast plasma data (Gosling/LANL) include four-level electron spectra, ion pseudondensities, average energies, and solar wind peak speeds and pseudodensities, at 5-minute resolution. The hot plasma (Frank, U. Iowa) algorithm outputs include proton densities, 10 keV electron fluxes, and energy range indicators, at 5-minute resolution. The fluxgate magnetometer data (Russell, UCLA) include 25 hourly parameters, plus the components of the magnetic field in spacecraft coordinates, at 1-minute resolution. The low-energy cosmic ray data (Hovestadt, MPI) include count rates of protons in three energy intervals between 0.17 and 20 MeV, plus those of alpha particles from 0.12 to 0.25 MeV and of Z>2 particles above 0.1 MeV, at 15-second resolution. The quasi-static electric field (Mozer, UCB) algorithm outputs indicate whether the experiment's electron guns were on or off during each 64-second interval. The plasma wave data (Gurnett, U. Iowa) include instantaneous samples from the 562 Hz filter channels of the electron and magnetic spectrum analysers, at 5-minute resolution. The plasma density data (Harvey, CESR) include indicators of the activity of the sounder and the propagation transmitters during each 64-second period. The energetic electron and proton algorithm outputs (Williams, APL) include both electron and proton differential fluxes in the 32 to 50 keV and the 80 to 126 keV energy ranges. These fluxes are taken in or near the spin-normal (nominally ecliptic) plane, at 5-minute resolution. The electron and proton experiment (K.Anderson, UCB) algorithm outputs include both electron and proton fluxes in the energy range 8 to 200 keV, at 5-minute resolution. The ion composition data (Sharp, Lockheed) include the cold plasma density and flags indicating the presence of high ion temperatures and bulk flow in the plasma, at 5-minute resolution. The Pool Tape Documentation (GSFC document X-692-77-129) (B29494 in NSSDC's Publications database) includes brief descriptions of the instruments, sometimes quite detailed, and also descriptions of the quick-look algorithms, also sometimes quite detailed. spase://SMWG/Person/H.Kent.Hills GeneralContact NSSDC Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?ds=SPMS-00147 spase://SMWG/Repository/NASA/NSSDC Offline Open NSSDC http://nssdc.gsfc.nasa.gov/nssdc/obtaining_data.html Binary 1 GB Calibrated spase://SMWG/Instrument/ISEE1/XFAN spase://SMWG/Instrument/ISEE1/LEPEDEA spase://SMWG/Instrument/ISEE1/MAG spase://SMWG/Instrument/ISEE1/LFEF spase://SMWG/Instrument/ISEE1/UCB ElectricField EnergeticParticles IonComposition MagneticField ThermalPlasma 1977-10-22T00:00:00 1987-11-26T00:00:00 PT1M Earth.Magnetosheath Earth.Magnetosphere Heliosphere.NearEarth These are preliminary data, typically recommended for event finding spase://SMWG/Observatory/ISEE1 ISEE 1 1977-102A International Sun-Earth Explorer-A Explorer 56 ISEE-A 2009-05-20T20:00:12Z The Explorer-class mother spacecraft, International Sun-Earth Explorer 1, was part of the mother/daughter/heliocentric mission (ISEE 1, ISEE 2, ISEE 3). The purposes of the mission were: (1) to investigate solar-terrestrial relationships at the outermost boundaries of the Earth's magnetosphere, (2) to examine in detail the structure of the solar wind near the Earth and the shock wave that forms the interface between the solar wind and the Earth's magnetosphere, (3) to investigate motions of and mechanisms operating in the plasma sheets, and (4) to continue the investigation of cosmic rays and solar flare effects in the interplanetary region near 1 AU. The three spacecraft carried a number of complementary instruments for making measurements of plasmas, energetic particles, waves, and fields. The mission thus extended the investigations of previous IMP spacecraft. The mother/daughter portion of the mission consisted of two spacecraft (ISEE 1 and ISEE 2) with station-keeping capability in the same highly eccentric geocentric orbit with an apogee of 23 Earth radii. During the course of the mission, the ISEE 1 and ISEE 2 orbit parameters underwent short-term and long-term variations due to solar and lunar perturbations. These two spacecraft maintained a small separation distance, and made simultaneous coordinated measurements to permit separation of spatial from temporal irregularities in the near-Earth solar wind, the bow shock, and inside the magnetosphere. By maneuvering ISEE 2, the inter-spacecraft separation as measured near the Earth's bow shock was allowed to vary between 10 km and 5000 km; its value is accurately known as a function of time and orbital position. The spacecraft were spin stabilized, with the spin vectors maintained nominally within 1 degree of perpendicular to the ecliptic plane, pointing north. The spin rates were nominally 19.75 rpm for ISEE 1 and 19.8 rpm for ISEE 2, so that there was a slow differential rotation between the two spacecraft. The ISEE 1 body-mounted solar array provided approximately 175 watts initially and 131 watts after three years, at 28 volts during normal operation. The ISEE 1 data rate was 4096 bps most of the time and 16384 bps during one orbit out of every five (with some exceptions). Both ISEE 1 and ISEE 2 re-entered the Earth's atmosphere during orbit 1518 on September 26, 1987. Seventeen of 21 on-board experiments were operational at the end. For instrument descriptions written by the investigators, see IEEE Trans. on Geosci. Electron., v. GE-16, no. 3, July 1978. spase://SMWG/Person/Keith.W.Ogilvie ProjectScientist NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=1977-102A Information about the ISEE 1 mission ISEE Heliosphere.NearEarth spase://SMWG/Instrument/ISEE1/LEPEDEA Low-Energy Proton and Electron Differential Energy Analyzer (LEPEDEA) LEPEDEA 2009-05-20T21:10:16Z This experiment was designed to study, by means of identical instrumentation on the mother/daughter spacecraft, the spatial and temporal variations of the solar wind and magnetosheath electrons and ions. Protons and electrons in the energy range from 1 eV to 45 keV were measured in 64 contiguous energy bands with an energy resolution (delta E/E) of 0.16. A quadrispherical low-energy proton and electron differential energy analyzer (LEPEDEA), employing seven continuous channel electron multipliers in each of its two (one for protons and one for electrons) electrostatic analyzers was flown on both the mother and the daughter spacecraft. All but 2% of the 4-pi-sr solid angle was covered for particle velocity vectors. A GM tube was also included, with a conical field of view of 40-deg full-angle, perpendicular to the spin axis. This detector was sensitive to electrons with E>45 keV, and to protons with E>600 keV. spase://SMWG/Person/H.Kent.Hills TechnicalContact spase://SMWG/Person/Charles.F.Kennel CoInvestigator spase://SMWG/Person/Vytenis.M.Vasyliunas CoInvestigator spase://SMWG/Person/Louis.A.Frank PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=1977-102A-03 Information about the Low-Energy Proton and Electron Differential Energy Analyzer (LEPEDEA) experiment on the ISEE 1 mission. ElectrostaticAnalyser Low-Energy Proton and Electron Differential Energy Analyzer (LEPEDEA) on ISEE 1 spase://SMWG/Observatory/ISEE1 spase://SMWG/Instrument/ISEE1/LFEF Quasi-static and low-frequency electric fields (0.1-200 mV/m, frequency < 1000Hz) 2009-05-20T21:10:16Z The objective of this experiment was to study quasi-static and low-frequency electric fields in the plasmasphere, magnetosphere, magnetosheath, and solar wind. Measurements were made of the potential difference between a pair of 8-cm diameter vitreous carbon spheres which were separated by 73.5 m and mounted on the ends of wire booms in the satellite spin plane. To attempt to overcome the spacecraft sheath (a potential problem which plagues all electric field detectors), an electron gun for changing the spacecraft potential was included, and all exposed spacecraft surfaces were made electrically conducting. The instrument was designed to be sensitive to fields from 0.1 to 200 mV/m in the frequency band of 0 to 12 Hz. The experiment also measured the electric field component of waves at frequencies below 1000 Hz. spase://SMWG/Person/Cynthia.A.Cattell GeneralContact spase://SMWG/Person/H.Kent.Hills TechnicalContact spase://SMWG/Person/Michael.C.Kelley CoInvestigator spase://SMWG/Person/Forrest.S.Mozer PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=1977-102A-06 Information about the Quasi-static and low-frequency electric fields (0.1-200 mV/m, frequency < 1000Hz) experiment on the ISEE 1 mission. DoubleSphere Quasi-static and low-frequency electric fields (0.1-200 mV/m, frequency < 1000Hz) on ISEE 1 spase://SMWG/Observatory/ISEE1 spase://SMWG/Instrument/ISEE1/MAG Fluxgate Magnetometer, Tri-axial 2009-05-20T21:10:16Z The magnetic fields investigation selected for ISEE 1 and 2 had as its principal objectives the study of the magnetic signatures of magnetospheric phenomena and magnetohydrodynamic waves in and around the magnetosphere, and to provide supporting data for other experiments on the spacecraft such as the electric field, particle and plasma wave investigations. In this triaxial fluxgate magnetometer, three ring-core sensors in an orthogonal triad were enclosed in a flipper mechanism at the end of the magnetometer boom. The electronics unit was on the main body of the spacecraft at the foot of the boom. The magnetometer had two operating ranges of +/- 8192 nT and +/- 256 nT in each vector component. The data were digitized and averaged within the instrument to provide increased resolution and to provide Nyquist filtering. There were two modes for the transmission of the averaged data. In the double-precision mode of operation, 16-bit samples of data were transmitted. This provided a maximum resolution of +/- 1/4 nT or 1/128 nT in th low-sensitivity and high-sensitivity ranges. In the single-precision mode, any 8 consecutive bits of the above 16 bits were selected by ground command for transmission and the telemetry bandwidths of the magnetometer were doubled. This bandwidth varied from 2 Hz for the low-telemetry-rate, double-precision experiment mode to 32 Hz for the high-telemetry-rate, single-precision experiment mode. Operation of this experiment was near nominal until spacecraft re-entry on September 26, 1987. Users of data from this experiment should be aware of the fact that the averaging of 12-bit samples to create 16-bit samples worked well in the spin plane, but in situations during which the field along the spin axis was quiet relative to the size of a digital window, the magnetometer returned only a 12-bit sample. This was particularly noticeable when the spacecraft was in the solar wind and the instrument was operated in its low gain (8192 nT) range, and when the spacecraft was in quiet regions of the magnetosphere in the low gain mode. The former situation limited the resolution of the field measured to 4 nT in the double precision mode in which the magnetometer usually was operated, and the latter situation created, as the spacecraft moved through the large gradient in the Earth's magnetic field, a stair step pattern of field changes of size 4 nT which may be mistaken for waves. Another operational anomaly was the saturation of a sensor during gain changes. At these times, the 3 components of the magnetic field were deduced from one spin tone and the field along the spin axis, limiting the temporal resolution of the instrument to below the spin frequency. Every effort was made to minimize zero level errors, clerical errors and other data processing anomalies within the available resources. However, these resources were very constrained and funding ceased before the entire submitted data set could be checked. It is expected that eventually quality checks of the entire database will be possible, but in the meantime, users of the ISEE-1 and 2 magnetometer data are requested to report all suspicions about data quality to the principal investigator, C. T. Russell, for verification. spase://SMWG/Person/Christopher.T.Russell PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=1977-102A&ex=4 Information about the Fluxgate Magnetometer, Tri-axial experiment on the ISEE 1 mission. Magnetometer Fluxgate Magnetometer, Tri-axial on ISEE 1 spase://SMWG/Observatory/ISEE1 spase://SMWG/Instrument/ISEE1/UCB ISEE 1 UCB Particle Detectors 2009-05-20T21:10:16Z This experiment was designed to determine, by using identical instrumentation (see 77-102B) on the mother/daughter spacecraft, the spatial extent, propagation velocity, and temporal behavior of a wide variety of particle phenomena. Electrons were measured at 2 and 6 keV and in two bands: 8 to 200 keV and 30 to 200 keV. Protons were measured at 2 and 6 keV and in three bands: 8 to 200 keV, 30 to 200 keV, and 200 to 380 keV. The 30 keV threshold could be commanded to 15 or 60 keV. Identical instrumentation on each spacecraft consisted of a pair of surface-barrier semiconductor-detector telescopes (one with a foil and one without a foil) and four fixed-voltage cylindrical electrostatic analyzers (two for electrons and two for protons). Channel multipliers were used as detectors with the fixed-voltage analyzers. The telescopes had a viewing cone with a 40-deg half-angle, oriented at about 20 deg to the spin axis. spase://SMWG/Person/Kinsey.A.Anderson PrincipalInvestigator NSSDC Master Catalog http://nssdc.gsfc.nasa.gov/nmc/experimentDisplay.do?id=1977-102A-10 spase://nssdc/instrument/1977-102A-10 ElectrostaticAnalyser Electron and Proton Fluxes in the Outer magnetosphere spase://SMWG/Observatory/ISEE1 spase://SMWG/Instrument/ISEE1/XFAN Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) 2009-05-20T21:10:16Z This experiment was designed, in conjunction with a similar instrument (77-102B-01) provided by G. Paschmann of Max Planck Institute for flight on the daughter spacecraft, to study the plasma velocity distribution and its spatial and temporal variations in the solar wind, bow shock, magnetosheath, magnetopause, magnetotail, and magnetosphere. The FPE consists of three high efficience 90 degree spherical section electrostatic analyzers using large secondary emitters and discrete dynode multipliers to detect analyzed particles. Two of them, viewing in opposite directions, produce complete 2D velocity distribution measurements of both protons and electrons every spacecraft revolution. A third FPE analyzer with a divided emitter measures 3D distributions at a slower rate. Protons from 50 eV to 40 keV and electrons from 5 eV to 20 keV were measured The experiment operated in two ranges, with energy resolution for the several steps in each range of 10% of the center energy level. The Solar Wind Experiment (SWE) measures solar wind ions. It is composed of two 150 degree spherical section analyzers using the same set of plates. The two acceptance fans are tilted with respect to each other so that 3D characteristics of the ion distributions can be derived. The ion experiment had degraded by April 1980 and the density values are suspected to be too low in later years. To protect the instrument, this experiment was turned off whenever the spacecraft was below 30,000 km. The Fast Plasma Experiment (FPE) had degraded by January 1978. spase://SMWG/Person/John.T.Gosling PrincipalInvestigator NSSDC's Master Catalog http://nssdc.gsfc.nasa.gov/database/MasterCatalog?sc=1977-102A&ex=1 Information about the Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) experiment on the ISEE 1 mission. ElectrostaticAnalyser Fast Plasma Experiment (FPE) and Solar Wind Ion Experiment (SWE) on ISEE 1 spase://SMWG/Observatory/ISEE1 spase://SMWG/Repository/NASA/NSSDC NSSDC 2008-08-26T21:02:30Z National Space Science Data Center spase://SMWG/Person/Edwin.J.Grayzeck.Jr GeneralContact spase://SMWG/Person/Edwin.V.Bell.II GeneralContact spase://SMWG/Repository/NSSDC spase://SMWG/Person/Michael.C.Kelley 2008-08-26T18:42:31Z Dr. Michael C. Kelley Cornell University

School of Electrical Engineering Cornell University 318 Rhodes Hall Ithaca NY 14853

mikek@ee.cornell.edu +1-607-254-5331 spase://SMWG/Person/John.T.Gosling Dr. John T. Gosling Los Alamos National Laboratory spase://SMWG/Person/Keith.W.Ogilvie 2007-05-30T15:38:05Z Dr. Keith W. Ogilvie NASA Goddard Space Flight Center

Code 673, Greenbelt, MD 20771, USA

keith.w.ogilvie@nasa.gov +1-301-286-5904 spase://SMWG/Person/Kinsey.A.Anderson Prof. Kinsey A. Anderson University of California, Berkeley spase://SMWG/Person/Louis.A.Frank 2008-08-26T18:45:59Z Prof. Louis A. Frank University of Iowa

Department of Physics and Astronomy University of Iowa Iowa City IA 52242

frank@iowasp.physics.uiowa.edu +1-319-335-1695 spase://SMWG/Person/Vytenis.M.Vasyliunas 2008-08-26T18:45:16Z Prof. Vytenis M. Vasyliunas Max-Planck-Institut fur Aeronomie

Max-Planck-Institut fur Aeronomie Postfach 20 37191 Katlenburg Germany

vasyliunas@linmpi.mpg.de +1-49-5556-401435 spase://SMWG/Person/Edwin.V.Bell.II Dr. Edwin V. Bell, II GSFC-Code 690.1 spase://SMWG/Person/Forrest.S.Mozer 2008-08-26T18:43:16Z Prof. Forrest S. Mozer University of California, Berkeley

Room 306 Space Science Laboratory University of California, Berkeley Berkeley CA 94720

mozer@sunspot.ssl.berkeley.edu +1-510-642-0549 spase://SMWG/Person/Charles.F.Kennel 2008-08-26T18:44:22Z Prof. Charles F. Kennel University of California, Los Angeles

Department of Physics University of California, Los Angeles 405 Hilgard Los Angeles CA 90095-1567

kennel@uclaph.ucla.edu +1-310-825-2052 spase://SMWG/Person/Christopher.T.Russell Dr. Christopher T. Russell University of California, Los Angeles spase://SMWG/Person/Cynthia.A.Cattell 2008-08-26T18:40:42Z Dr. Cynthia A. Cattell University of Minnesota

Tate Laboratory of Physics School of Physics and Astronomy University of Minnesota 116 Church Street SE Minneapolis MN 55455-0112

cattell@belka.spa.umn.edu +1-612-626-2029 spase://SMWG/Person/Edwin.J.Grayzeck.Jr Dr. Edwin J. Grayzeck, Jr. GSFC-Code 690.1 spase://SMWG/Person/H.Kent.Hills 2008-08-26T18:41:43Z Dr. H. Kent Hills GSFC-Code 690.1

GSFC-Code 690.1 QSS Group Inc

hills@nssdc.gsfc.nasa.gov +1-301-286-1771