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Data set records contain fluxes of protons in 5 energy ranges (4-13, 13-27, 27-37, 37-51, >51 MeV), alpha particles in 6 energy ranges (2-4, 4-13, 13-27, 27-37, 37-48, >48 MeV/n), and electrons in 2 ranges (0.3-0.8, 0.8-2.0 MeV). The fluxes are averaged over intervals of approximately one hour. Each "data record" (having ending CR and/or LF) spans 4-5 hours and has 10 time-overlapping segments. Each segment has averaging start and stop times plus words for 13 fluxes and words for the statistical uncertainties in the 13 fluxes. However, most words in a given segment have fill values, such that good values for a given flux (species and energy range) and its uncertainty appear only in a minority of the segments. No spacecraft position information is included. Data are from the E6 experiment on Helios 2.
Please acknowledge the P.I., Horst Kunow at Universitat Kiel
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | Dr. Horst W. Kunow |
The start and stop times of the flux averages, each given as four words: year, day of year, hour, minute
The start and stop times of the flux averages, each given as four words: year, day of year, hour, minute. These are given in each of the 10 time segments for each data record
Fluxes of protons in 5 energy ranges (4-13, 13-27, 27-37, 37-51, >51 MeV) and associated statistical uncertainties for each flux.
Fluxes of protons in 5 energy ranges (4-13, 13-27, 27-37, 37-51, >51 MeV) and associated statistical uncertainties for each flux. These are given in each of the 10 time segments for each data record. (See general description above.)
Fluxes of alpha particles in 6 energy ranges (2-4, 4-13, 13-27, 27-37, 37-48, >48 MeV/n) and associated statistical uncertainties for each flux.
Fluxes of alpha particles in 6 energy ranges (2-4, 4-13, 13-27, 27-37, 37-48, >48 MeV/n) and associated statistical uncertainties for each flux. These are given in each of the 10 time segments for each data record. (See general description above.)
Fluxes of electrons in 2 energy ranges (0.3-0.8, 0.8-2.0 MeV) and associated statistical uncertainties for each flux.
Fluxes of electrons in 2 energy ranges (0.3-0.8, 0.8-2.0 MeV) and associated statistical uncertainties for each flux. These are given in each of the 10 time segments for each data record. (See general description above.)
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The objective of the experiment (E6) was to study high-energy, charged, cosmic-ray particles of solar, planetary, and galactic origin in interplanetary space. Protons and alpha particles with energies >1.3 MeV/nucleon, and electrons >0.3 MeV were measured within interplanetary space over the range from 0.3 to 1.0 AU. The instrument, a particle telescope with a 55-deg field of view, consisted of five semiconductor detectors, one sapphire Cerenkov counter, and one scintillation counter, all enclosed by an anticoincidence cylinder. The telescope was calibrated prior to launch using radioactive sources, particle accelerators, and ground-level muons. It measured protons and alpha particles in six channels (1.3-3.3, 3.3-13, 13-27, 27-37, 37-45, and >45 MeV/nucleon) and electrons in five energy channels (0.3-0.8, 0.8-2, 2-3, 3-4, and >4 MeV). For more detail see pp. 253-257 of Raumfahrtforschung, v. 19, n. 5, 1975.
Information about the Cosmic Ray Particle experiment on the Helios-B mission.
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | Dr. Horst W. Kunow |
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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 |