HR: 08:15h
AN: SM21C-02    [Abstracts]
TI: Mirror Mode Waves in the Jovian Magnetosheath
AU: * Joy, S P
EM: sjoy@igpp.ucla.edu
AF: University of California, Los Angeles Institute of Geophysics and Planetary Physics, 405 Hilgard Ave, Los Angeles, CA 90095-1567 United States
AU: * Joy, S P
EM: sjoy@igpp.ucla.edu
AF: University of California, Los Angeles Dept. of Earth and Space Sciences, 405 Hilgard Ave, Los Angeles, CA 90095-2567 United States
AU: Kivelson, M G
EM: mkivelson@igpp.ucla.edu
AF: University of California, Los Angeles Institute of Geophysics and Planetary Physics, 405 Hilgard Ave, Los Angeles, CA 90095-1567 United States
AU: Kivelson, M G
EM: mkivelson@igpp.ucla.edu
AF: University of California, Los Angeles Dept. of Earth and Space Sciences, 405 Hilgard Ave, Los Angeles, CA 90095-2567 United States
AU: Paterson, W
EM: william.paterson@uiowa.edu
AF: Hampton Univ, Center Atmospheric Sciences, Hampton, VA 23668
AU: Schwarzl, H
EM: hannes@igpp.ucla.edu
AF: University of California, Los Angeles Institute of Geophysics and Planetary Physics, 405 Hilgard Ave, Los Angeles, CA 90095-1567 United States
AU: Vo, S
EM: svo@igpp.ucla.edu
AF: University of California, Los Angeles Institute of Geophysics and Planetary Physics, 405 Hilgard Ave, Los Angeles, CA 90095-1567 United States
AB: Mirror modes waves are commonly observed in planetary magnetosheaths, cometary sheaths, and other plasmas with anisotropic pressure distributions. In this paper we present results derived from observations from many spacecraft that have sampled the Jovian magnetosheath over a wide range of radial distances and local times (Pioneer 10 & 11, Voyager 1 & 2, Ulysses, and Galileo). Several magnetic field signatures are associated with mirror mode waves at Jupiter. The are {\it spikes} where the field strength is briefly elevated above a slowly varying background level, {\it dips} where the opposite occurs, and {\it other} mirror mode waves where there is no clearly defined background field in the wave region. Here we report on the radial distance, local time, and spatial scale size distributions of each of these three magnetic structures. We examine the plasma parameters (Beta, number density, temperature, velocity) associated with each of these magnetic waveforms. We examine the relationship between the properties of the ambient plasma and the presence of waves and their structure.
DE: 7871 Waves and instabilities
DE: 6220 Jupiter
DE: 2728 Magnetosheath
DE: 2752 MHD waves and instabilities
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting