Data Set Information
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| DATA_SET_NAME |
ULY JUP COSPIN HIGH ENERGY TELESCOPE HIGH RES. PARTICLE FLUX
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| DATA_SET_ID |
ULY-J-COSPIN-HET-3-RDR-FLUX-HIRES-V1.0
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| NSSDC_DATA_SET_ID |
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| DATA_SET_TERSE_DESCRIPTION |
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| DATA_SET_DESCRIPTION |
Data ==== HET data record format ---------------------- Column 1: Date/time in format yyyy-mm-ddThh:mm:ss.sssZ Column 2: Accumulation time (second) for H1-H9 Column 3: H1 counting rate (c/s) Column 4: H2 counting rate (c/s) Column 5: H3 counting rate (c/s) Column 6: H4 counting rate (c/s) Column 7: H5 counting rate (c/s) Column 8: H6 counting rate (c/s) Column 9: H7 counting rate (c/s) Column 10: H8 counting rate (c/s) Column 11: H9 counting rate (c/s) [please note that time-stamp and record format have been changed by the PDS/PPI Node for the sake of consistency with other data sets found on this volume] A caveat is that during most of the Jupiter flyby, the counting rate logic was swamped by the extremely high intensity of electrons contained in the magnetosphere. As a result, we believe that the most reliable interpretation of the counting rates is that they become effectively measures of the integral intensity above the minimum energy required for an electron to penetrate to the most deeply buried detector required by the counting rate logic. For example, the H4 counting rate, which is nominally defined by the coincidence D1 D2 D4 K1 N[K4 A S (H)] becomes the integral intensity of all electrons with sufficient energy to reach K1, which, by the table below, based on the Berger and Seltzer tables and the thicknesses of the D1-D6 detectors, is ~2.7 MeV. The minimum electron energies required to trigger the counting rates, based simply on energy required to penetrate to the deepest detector and trigger its discriminator are as follows. For detectors beyond the midpoint of the telescope, we have assumed that there is sufficient material (instrument and spacecraft) behind the telescope that the easiest access to the detector is still through the front of the telescope. This may not be a good assumption. H1 ~0.5 MeV H2 ~2.6 MeV (higher level discriminators on D1 and D2 H3 ~1.5 MeV required) H4 ~2.7 MeV H5 ~8.9 MeV H6 ~1.2 MeV H7 ~2.7 MeV H8 ~1.5 MeV H9 ~16 MeV The detailed coincidence logic defining these counting rates is given in [SIMPSONETAL1992A]. As indicated by the ~, these energies are very approximate. Our assumption is that essentially all the counting rates, even those such as H2 designed to discriminate against electrons, were dominated by electrons inside the magnetosphere. One additional word of explanation is required. In an ill-advised attempt to configure the HET to a mode to minimize the effects of the expected high counting rates on our slow logic, from approximately 1206 UT day 32 until approximately 0018 UT day 34, the HET S detector High Voltage was turned off, effectively turning off S, and the D1 detector was replaced by D3 in the counting rate logic. (Commands C1 and C9 as described in Table 8 of [SIMPSONETAL1992A].) The intent was to remove from the logic those detectors expected to be in near- saturation throughout the flyby, and thus to make the counting rates more interpretable. The change was effected before crossing the bowshock and magnetopause in order to establish a base-line in the new configuration prior to encountering the expected high fluxes in the magnetosphere. The actual effect turned out to be to increase the background in most of the counting rates to such a high level that features such as up- stream particles escaping from the magnetosphere were completely obscured. After about a day and a half in this mode, it was decided to return to normal mode, and we remained in normal mode for the remainder of the flyby.
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| DATA_SET_RELEASE_DATE |
1998-05-01T00:00:00.000Z
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| START_TIME |
1992-01-25T12:00:00.864Z
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| STOP_TIME |
1992-02-14T11:59:57.411Z
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| MISSION_NAME |
ULYSSES
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| MISSION_START_DATE |
1990-10-06T12:00:00.000Z
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| MISSION_STOP_DATE |
N/A (ongoing)
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| TARGET_NAME |
JUPITER
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| TARGET_TYPE |
PLANET
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| INSTRUMENT_HOST_ID |
ULY
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| INSTRUMENT_NAME |
COSPIN-HIGH ENERGY TELESCOPE
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| INSTRUMENT_ID |
COSPIN-HET
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| INSTRUMENT_TYPE |
HIGH ENERGY PARTICLE DETECTOR
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| NODE_NAME |
planetary plasma interactions
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| ARCHIVE_STATUS |
ARCHIVED
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| CONFIDENCE_LEVEL_NOTE |
Confidence Level Overview ========================= Some confidence level information provided in Data Set Overview. For more information regarding the confidence level of this data set please contact: JOHN A. SIMPSON Laboratory for Astrophysics and Space Research University of Chicago 933 East 56th Street Chicago, IL 60637 USA Phone: 1-312-702-7670 Fax: 1-312-702-6645 Internet: simpson@odysseus.uchicago.edu
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| CITATION_DESCRIPTION |
Simpson, J.A., ULY-J-COSPIN-HET-3-RDR-FLUX-HIRES-V1.0, ULY JUP COSPIN HIGH ENERGY TELESCOPE HIGH RES. PARTICLE FLUX, NASA Planetary Data System, 1998.
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| ABSTRACT_TEXT |
ULY JUP COSPIN HIGH ENERGY TELESCOPE HIGH RES. PARTICLE FLUX
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| PRODUCER_FULL_NAME |
JOHN A. SIMPSON
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| SEARCH/ACCESS DATA |
Planetary Plasma Interactions Website
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