This page summarizes information about the selected resource and its origin based on SPASE metadata.
SPASE version 2.0.0
this set contains daily averaged PHA derived fluxes of protons (34.1-125.0, 125.0-320.0, 320.0-2100.0, >2100.0 MeV) alpha particles (34.2-125.0, 125.0-320.0, 320.0-2100.0, >2100.0 MeV/n) and electrons (2.5-7.0 Mev, 2.5 GV) and the Poisson uncertainties in those fluxes
The README file at the Ulysses Data System (UDS) describes the format of the ASCII data files containing daily average proton, helium and electron PHA derived count rates for the COSPIN Kiel Electron Telescope (KET), and caveats for their use.
Please acknowlegde the COSPIN PI (R.B. McKibben), the KET Co-PI (B. Heber) and the UDS and/or NSSDC
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | Dr. R. Bruce McKibben |
| 2. | CoInvestigator | Dr. Bernd Heber |
| 3. | ArchiveSpecialist | Dr. Cecil Tranquille |
ASCII data file containing all Ulysses COSPIN/KET daily average proton, helium and electron PHA derived count rates.
B. Heber, CAU Kiel
Time for the record given in year, day of year, hour, min, seconds and coverage in percent. The given time represents the start of the averaging interval.
| Index | Name | Valid min | Valid max |
|---|---|---|---|
| 1 | Year | 1990 | 2008 |
| 2 | Day of year | 1 | 366 |
| 3 | Hour of day | 0 | 23 |
| 4 | Minute of hour | 0 | 59 |
| 5 | Seconds of minute | 0 | 59 |
| 6 | Coverage | 0 | 100 |
KET daily average PHA derived proton count rates between 34.1 and 125.0 MeV
None
error in KET daily average PHA derived proton count rates between 34.1 and 125.0 MeV
None
KET daily average PHA derived proton count rates between 125.0 and 320.0 MeV
None
error in KET daily average PHA derived proton count rates between 125.0 and 320.0 MeV
None
KET daily average PHA derived proton count rates between 320.0 and 2100.0 MeV
None
error in KET daily average PHA derived proton count rates between 320.0 and 2100.0 MeV
None
KET daily average PHA derived proton count rates >2100.0 MeV
None
error in KET daily average PHA derived proton count rates >2100.0 MeV
None
KET daily average PHA derived helium count rates between 34.2 and 125.0 MeV/n
None
error in KET daily average PHA derived helium count rates between 34.2 and 125.0 MeV/n
None
KET daily average PHA derived helium count rates between 125.0 and 320.0 MeV/n
None
error in KET daily average PHA derived helium count rates between 125.0 and 320.0 MeV/n
None
KET daily average PHA derived helium count rates between 320.0 and 2100.0 MeV/n
None
error in KET daily average PHA derived helium count rates between 320.0 and 2100.0 MeV/n
None
KET daily average PHA derived helium count rates >2100.0 MeV/n
None
error in KET daily average PHA derived helium count rates >2100.0 MeV/n
None
KET daily average PHA derived electron count rates between 2.5 and 7.0 MeV
None
error in KET daily average PHA derived electron count rates between 2.5 and 7.0 MeV
None
KET daily average PHA derived 2.5 GeV electron count rates
None
error in KET daily average PHA derived 2.5 GeV electron count rates
None
daily average KET A01 detector counting rate
Rate channel A01 includes all particles depositing energy greater than the minimum discriminator level.
SPASE version 2.0.0
Kiel Electron Telescope (KET): ~3-200 MeV electrons and ~3-2100 MeV/n protons and He using a Large dE/dx vs. E and cerenkov telescope with pha capability optimized for studies of high energy electrons, protons, and helium.
KET is one of five instruments that make up the COSPIN suite on the Ulysses spacecraft. KET was built, and primary data analysis is maintained, by Christian Albrechts University, Kiel, Germany
Information about the KET experiment on the Ulysses mission.
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | Dr. R. Bruce McKibben |
| 2. | CoInvestigator | Dr. Bernd Heber |
SPASE version 2.0.0
The primary objectives of Ulysses, formerly the International Solar Polar Mission (ISPM), are to investigate, as a function of solar latitude, the properties of the solar wind and the interplanetary magnetic field, of galactic cosmic rays and neutral interstellar gas, and to study energetic particle composition and acceleration. The 55 kg payload includes two magnetometers, two solar wind plasma instruments, a unified radio/plasma wave instrument, three energetic charged particle instruments, an interstellar neutral gas sensor, a solar X-ray/cosmic gamma-ray burst detector, and a cosmic dust sensor. The communications systems is also used to study the solar corona and to search for gravitational waves. Secondary objectives included interplanetary and planetary physics investigations during the initial Earth-Jupiter phase and investigations in the Jovian magnetosphere. The spacecraft used a Jupiter swingby in Feb. 1992 to transfer to a heliospheric orbit with high heliocentric inclination, and will pass over the rotational south pole of the sun in mid-1994 at 2 AU, and over the north pole in mid-1995. A second solar orbit will take Ulysses again over the south and north poles in years 2000 and 2001, respectively. The spacecraft is powered by a single radio-isotope generator. It is spin stabilized at a rate of 5 rpm and its high-gain antenna points continuously to the earth. A nutation anomaly after launch was controlled by CONSCAN. The original mission planned for two spacecraft, one built by ESA and the other by NASA. NASA cancelled its spacecraft in 1981.
JPL's primary website for the Ulysses mission. Links to all of the experiment subpages exist here.
| Role | Person | |
|---|---|---|
| 1. | Project scientist | Dr. Edward J. Smith |
| 2. | Project scientist | Dr. Richard G. Marsden |
SPASE version 2.0.0
SPASE version 2.0.0
SPASE version 2.0.0
SPASE version 2.0.0
SPASE version 2.0.0