Properties of ultra low frequency upstream waves at Venus and Saturn: A comparison

Details Properties of ultra low frequency upstream waves at Venus and Saturn: A comparison Properties of ultra low frequency upstream waves at Venus and Saturn: A comparison

Aug 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995adspr..16..143o&link_type=abstract

Advances in Space Research (ISSN 0273-1177), vol. 16, no. 4, p. (4)143-(4)148

Astronomy and Astrophysics

Astronomy

Extremely Low Frequencies, Interplanetary Magnetic Fields, Saturn (Planet), Solar Wind, Venus (Planet), Wave Dispersion, Astronomical Models, Mach Number, Magnetic Compression, Magnetohydrodynamic Waves, Polarization (Spin Alignment), Power Spectra, Proton Beams, Radio Astronomy, Shock Waves

Scientific paper

The 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.

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