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The coronal-sounding experimentThe main science objective of the Ulysses Solar Corona Experiment is to derive the plasma parameters of the solar atmosphere using established coronal-sounding techniques. Applying appropriate model assumptions, the 3D electron density distribution will be determined from dual-frequency ranging and Doppler measurements recorded at the NASA Deep Space Network during the solar conjunctions. Multi-station observations will be used to derive the plasma bulk velocity at solar distances where the solar wind is expected to undergo its greatest acceleration. As a secondary objective profiting from the favorable geometry during Jupiter encounter, radio-sounding measurements will yield a unique cross-scan of the electron density in the Io Plasma Torus.
Document ID
19920041695
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Bird, M. K.
(Bonn, Universitaet Federal Republic of Germany, United States)
Asmar, S. W.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA, United States)
Brenkle, J. P.
(JPL Pasadena, CA, United States)
Edenhofer, P.
(Bochum, Ruhr-Universitaet Federal Republic of Germany, United States)
Paetzold, M.
(DLR, Institut fuer Hochfrequenztechnik, Wessling Federal Republic of Germany, United States)
Volland, H.
(Bonn, Universitaet Federal Republic of Germany, United States)
Date Acquired
August 15, 2013
Publication Date
January 1, 1992
Publication Information
Publication: Astronomy and Astrophysics Supplement Series
Volume: 92
Issue: 2 Ja
ISSN: 0365-0138
Subject Category
Spacecraft Instrumentation
Accession Number
92A24319
Funding Number(s)
CONTRACT_GRANT: BMFT-50-ON-9104
Distribution Limits
Public
Copyright
Other

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