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Properties of ultra low frequency upstream waves at Venus and Saturn: A comparisonThe upstream regions of all planets, except Pluto, have been investigated, using in situ spacecraft measurements and a variety of analysis techniques. The detailed studies at Earth indicate that these waves are generated locally in the magnetically connected solar wind by the interaction with ions backstreaming from the shock. However, since the properties of the solar wind vary with heliocentric distance and since properties of planetary shocks depend on plasma beta, interplanetary magnetic field (IMF) spiral angle and Mach number, the amount of heating, acceleration efficiencies, etc. significantly change with heliocentric distance. In turn the waves seen at each planet propagate not in the same but different (physical) propagation modes. In this paper we compare the ULF wave observations at an outer and an inner planet. We use the results of the ratio, quantites easily derivable with sufficient accuracy at each planet. We use the full electromagnetic dispersion relation for comparison with theoretical predictions.
Document ID
19950055855
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Orlowski, D. S.
(University of California, Los Angeles, CA US, United States)
Russell, C. T.
(University of California, Los Angeles, CA US, United States)
Krauss-Varban, D.
(University of California, San Diego, CA US, United States)
Omidi, N.
(University of California, San Diego, CA US, United States)
Date Acquired
August 16, 2013
Publication Date
August 1, 1995
Publication Information
Publication: Advances in Space Research
Volume: 16
Issue: 4
ISSN: 0273-1177
Subject Category
Astrophysics
Accession Number
95A87454
Funding Number(s)
CONTRACT_GRANT: NAGW-2886
CONTRACT_GRANT: NAGW-2139
Distribution Limits
Public
Copyright
Other

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