This page summarizes information about the selected resource and its origin based on SPASE metadata.
SPASE version 2.0.0
This data set contains 10-Minute averages of: (a) spin-integrated fluxes of protons (0.9-1.2, 1.2-3.0, 1.8-3.8, 3.8-8.0 and 8.0-19.0 MeV), alpha particles (1.0-5.0, 1.9-3.7, 3.7-8.4 and 8.4-19.0 MeV/n), Li,Be,B nuclei (1.9-4.9 and 4.9-26 MeV/n), C,N,O nuclei (2.6-7.1 and 7.1-39 MeV/n)MeV/n), Z GE 10 nuclei (3.0-9.0 MeV/n), 10 LE Z LE 20 nuclei (9.0-50 MeV/n) and Z GE 20 nuclei (12-75 MeV/n); (b) 8-sectored proton fluxes (1.8-3.8 and 3.8-8.0 MeV); (c) count rates of electrons (0.3-1.0 MeV) and D1, D2, D3, D4 and D5 single detector sensors
The README file at the Ulysses Data System (UDS) describes the format of the ASCII data files containing 10-minute average ion and electron fluxes and detector count rates for the COSPIN Low Energy Telescope (LET), and caveats for their use.
Please acknowlegde the COSPIN PI (R.B. McKibben), the lead LET CoI (R.G. Marsden) and the UDS and/or NSSDC
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | Dr. R. Bruce McKibben |
| 2. | CoInvestigator | Dr. Richard G. Marsden |
| 3. | ArchiveSpecialist | Dr. Cecil Tranquille |
Parent directory containing compressed Ulysses COSPIN/LET 10-minute average rates data organised in daily ASCII files ucosletrYYDOY.dat (YY and DOY are the two digit year and the day of year, respectively) grouped together into yearly files (cosletYY.zip, where YY is the two digit year).
R.G. Marsden, ESA/ESTEC
Time for the record given in year, day of year, hour, min, and seconds. 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 |
10-minute average LET spin-averaged proton fluxes between 0.9 and 1.2 MeV
Rate channel L1 (which nominally responds to protons in the energy range 0.9-1.2 MeV) is derived from a single detector measurement, and as such is sensitive to penetrating particles which lose part of their energy in the detector. The background contribution depends on the energy spectrum of the incident particle population, being negligible for (differential) energy spectral slopes of -3.5 or steeper, increasing to 80% of the total counts for a slope of -1.0 or harder.
10-minute average LET spin-averaged proton fluxes between 1.2 and 3.0 MeV
Rate channel L2 is derived from a single detector measurement, and the nominal energy response to protons (1.2-3.0 MeV) is approximate.
10-minute average LET spin-averaged proton fluxes between 1.8 and 3.8 MeV
None
10-minute average LET proton fluxes in spin sector 1 (of 8) between 1.8 and 3.8 MeV
None
10-minute average LET proton fluxes in spin sector 2 (of 8) between 1.8 and 3.8 MeV
None
10-minute average LET proton fluxes in spin sector 3 (of 8) between 1.8 and 3.8 MeV
None
10-minute average LET proton fluxes in spin sector 4 (of 8) between 1.8 and 3.8 MeV
None
10-minute average LET proton fluxes in spin sector 5 (of 8) between 1.8 and 3.8 MeV
None
10-minute average LET proton fluxes in spin sector 6 (of 8) between 1.8 and 3.8 MeV
None
10-minute average LET proton fluxes in spin sector 7 (of 8) between 1.8 and 3.8 MeV
None
10-minute average LET proton fluxes in spin sector 8 (of 8) between 1.8 and 3.8 MeV
None
10-minute average LET spin-averaged proton fluxes between 3.8 and 8.0 MeV
None
10-minute average LET proton fluxes in spin sector 1 (of 8) between 3.8 and 8.0 MeV
None
10-minute average LET proton fluxes in spin sector 2 (of 8) between 3.8 and 8.0 MeV
None
10-minute average LET proton fluxes in spin sector 3 (of 8) between 3.8 and 8.0 MeV
None
10-minute average LET proton fluxes in spin sector 4 (of 8) between 3.8 and 8.0 MeV
None
10-minute average LET proton fluxes in spin sector 5 (of 8) between 3.8 and 8.0 MeV
None
10-minute average LET proton fluxes in spin sector 6 (of 8) between 3.8 and 8.0 MeV
None
10-minute average LET proton fluxes in spin sector 7 (of 8) between 3.8 and 8.0 MeV
None
10-minute average LET proton fluxes in spin sector 8 (of 8) between 3.8 and 8.0 MeV
None
10-minute average LET spin-averaged proton fluxes between 8.0 and 19.0 MeV
Rate channel L21 (which nominally responds to protons in the energy range 9-19 MeV) is also sensitive to higher-energy particles which lose part of their energy in the telescope structure. As in the case of L1, the background contribution depends on the energy spectrum of the incident particle population, being negligible for (differential) energy spectral slopes of -2.0 or steeper, increasing to 80% of the total counts for a slope of +0.75 or harder.
10-minute average LET spin-averaged alpha fluxes between 1.0 and 5.0 MeV/n
Rate channel L22 is derived from a single detector measurement, and the nominal energy response to alpha particles (1.0-5.0 MeV/n) is approximate.
10-minute average LET spin-averaged alpha fluxes between 1.9 and 3.7 MeV/n
None
10-minute average LET spin-averaged alpha fluxes between 3.7 and 8.4 MeV/n
None
10-minute average LET spin-averaged alpha fluxes between 8.4 and 19.0 MeV/n
Rate channel L25 (which nominally responds to alpha particles in the energy range 8.4-19.0 MeV/n) is also sensitive to higher energy particles that lose part of their energy in the telescope structure. As in the case of L21, the background contribution depends on the energy spectrum of the incident particle population (negligible for differential energy spectral slopes of -2.0 or steeper).
10-minute average LET spin-averaged Li, Be and B fluxes between 1.9 and 4.9 MeV/n
Rate channel L26 suffers from background due to pulse pile-up for proton fluxes in L2 greater than 10 protons/cm^2/s/sr/MeV.
10-minute average LET spin-averaged Li, Be and B fluxes between 4.9 and 26.0 MeV/n
Rate channel L27 suffers from background due to pulse pile-up for proton fluxes in L2 greater than 30 protons/cm^2/s/sr/MeV.
10-minute average LET spin-averaged C, N and O fluxes between 2.6 and 7.1 MeV/n
The energy for rate channel L28 is approximate (species dependent).
10-minute average LET spin-averaged C, N and O fluxes between 7.1 and 39.0 MeV/n
The energy for rate channel L29 is approximate (species dependent).
10-minute average LET spin-averaged Z GE 10 fluxes between 3.0 and 9.0 MeV/n
The energy for rate channel L30 is approximate (species dependent).
10-minute average LET spin-averaged 10 LE Z LE 20 fluxes between 9.0 and 50.0 MeV/n
The energy for rate channel L31 is approximate (species dependent).
10-minute average LET spin-averaged Z GE 20 fluxes between 12.0 and 75.0 MeV/n
The energy for rate channel L32 is approximate (species dependent).
10-minute average LET spin-averaged electron fluxes between 0.3 and 1.0 MeV
The energy range for rate channel L33 is approximate. L33 suffers from background from the RTG and GCR.
10-minute average LET D1 detector counting rate
Rate channel L34 includes all particles depositing energy greater than the minimum discriminator level.
10-minute average LET D2 detector counting rate
Rate channel L35 includes all particles depositing energy greater than the minimum discriminator level.
10-minute average LET D3 detector counting rate
Rate channel L35 includes all particles depositing energy greater than the minimum discriminator level.
10-minute average LET D4 detector counting rate
Rate channel L37 includes all particles depositing energy greater than the minimum discriminator level.
10-minute average LET D5 detector counting rate
Rate channel L38 includes all particles depositing energy greater than the minimum discriminator level.
SPASE version 2.0.0
Low Energy Telescope (LET): ~1-20 MeV/n P, He, and heavier nuclei using a dE/dx vs. E telescope with pha capability
LET is one of five instruments that make up the COSPIN suite on the Ulysses spacecraft. LET was built, and primary data analysis is maintained, by ESTEC, Noordwijk, The Netherlands
Information about the LET experiment on the Ulysses mission.
| Role | Person | |
|---|---|---|
| 1. | Principal investigator | Dr. R. Bruce McKibben |
| 2. | CoInvestigator | Silvia Dalla |
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