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Data set records contain hourly count rates of protons and electrons in 16 energy ranges (protons: 15 differential channels between 21 and 677 keV, plus >677 keV; electrons: 15 differential channels between 17 and 835 keV, plus >835 keV), each in 16 22.5 deg azimuthal sectors. Accumulation times for each count rate are also given. No spacecraft position information is included. Data are from the E8 experiment on Helios 2.
Please acknowledge the P.I., Erhard Keppler of Max Planck Institure, Lindau
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | spase://SMWG/Person/Erhard.Keppler |
The start times of the count rate averages, given as five words: hours since start of 1974, year, day of year, hour, minute. Values of the last one is uniformly zero.
16-sectored count rates of electrons in 16 energy ranges (17-22, 22-28, 28-36, 36-46, 46-58, 58-74, 74-92, 93-120, 120-153, 153-201, 201-248, 248-298, 300-412, 412-525, 525-835, >835 keV).
Count rates of electrons in 16 energy ranges for each of 16 azimuthal sectors. Data cycle through energies for first sector, then repeats for second sector, etc.
Accumulation times for each of the preceding 16x16 electron count rates.
The accumulation time for a given count rate immediately follows its associated count rate in the data records.
16-sectored count rates of electrons in 16 energy ranges (21-27, 27-35, 35-44, 44-56, 56-71, 71-90, 90-110, 110-137, 137-174, 174-222, 222-279, 279-353, 353-444, 444-563, 563-677, >677 keV).
Count rates of protonsons in 16 energy ranges for each of 16 azimuthal sectors. Data cycle through energies for first sector, then repeats for second sector, etc.
Accumulation times for each of the preceding 16x16 proton count rates.
The accumulation time for a given count rate immediately follows its associated count rate in the data records.
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The objective of the experiment (E8) was to study the origin and the distribution mechanism of low-energy electrons and protons. The instrument, a magnetic spectrometer, consisted of six semiconductor detectors with the field of view in the plane of the ecliptic. Species separation was achieved by an inhomogeneous magnetic field oriented perpendicular to the particle path. Four electron and two proton detectors measured electrons from 17 to 835 keV and protons from 21 to 677 keV. The proton measurements were made with a two-detector telescope employing coincidence and anticoincidence logic. Both particle species were measured in 16 energy channels through pulse-height analysis. For further information see pp. 261-263 of Raumfahrtforschung, v. 19, n. 5, 1975.
The NSSDC Data Set Catalog contains within itself a PI-generated detailed description of the experiment and data handling.
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | spase://SMWG/Person/Erhard.Keppler |
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This spacecraft was one of a pair of deep-space probes developed by the Federal Republic of Germany (FRG) in a cooperative program with NASA. Experiments were provided by scientists from both FRG and the U.S. NASA supplied the Titan/Centaur launch vehicle. The spacecraft was equipped with two booms and a 32-m electric dipole. The payload consisted of a fluxgate magnetometer; electric and magnetic wave experiments, which covered various bands in the frequency range 6 Hz to 3 MHz; charged particle experiments, which covered various energy ranges starting with solar wind thermal energies and extending to 1 GeV; a zodiacal light experiment; and a micrometeoroid experiment. The purpose of the mission was to make pioneering measurements of the interplanetary medium from the vicinity of the earth's orbit to 0.3 AU. The spacecraft was spin stabilized with the spin axis normal to the ecliptic, and a nominal spin rate of 1 rps. The outer surface was coated with a conductive material, resulting in a plasma-sheath potential of typically 5 eV. Sheath-related coupling caused by the spacecraft antennae produced interference with the wave experiments, but the character of the interference was different from that observed on the Helios-A spacecraft. The spacecraft was capable of being operated at bit rates of from 4096 to 8 bps, variable by factors of two. While the spacecraft was moving to perihelion, it was generally operated from 64 to 256 bps; near 0.3 AU, it was operated at higher bit rates. Because of difficulty encountered with the high-gain antenna, and scheduling conflicts with Viking, relatively fewer high-bit-rate data were obtained from Helios-B than were available from Helios-A. Instrument descriptions written by the experiments are published (some in German, some in English) in the journal Raumfahrtforschung, v. 19, n. 5, 1975.
Information about the Helios-B mission
| Role | Person | |
|---|---|---|
| 1. | Project scientist | Dr. James H. Trainor |
| 2. | Project scientist | Dr. Herbert Porsche |
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Space Physics Data Facility
Space Physics Data Facility
| Role | Person | |
|---|---|---|
| 1. | General contact | Ms. Tamara J. Kovalick |
| 2. | Technical contact | Mr. Robert M. Candey |
| 3. | Project scientist | Dr. Robert E. McGuire |