HR: 0800h
AN: SH21B-0420    [Abstracts]
TI: Solar Coronal Magnetic Fields From Cassini Faraday Rotation
AU: * Jensen, E
EM: ejensen@igpp.ucla.edu
AF: Univerity of California Los Angeles, Institue of Geophysics and Planetary Physics 405 Hilgard Avenue, Los Angeles, CA 90095-1567 United States
AU: Bird, M K
EM: mbird@astro.uni-bonn.de
AF: Universitat Bonn, Radioastron. Institut. Auf dem Huegel 71 53121 Bonn, Bonn, Ger 53121
AU: Amar, S
AF: Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109 United States
AU: Iess, L
AF: University of Rome, Rome, Rome, Ita 12345
AU: Luhmann, J G
EM: jgluhman@ssl.berkeley.edu
AF: University of California Berkeley, Space Sciences Laboratory, Berkeley, CA 94720-7450 United States
AU: Anderson, J D
EM: anderson@jpl.nasa.gov
AF: Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109 United States
AU: Russell, C T
EM: ctrussell@igpp.ucla.edu
AF: Univerity of California Los Angeles, Institue of Geophysics and Planetary Physics 405 Hilgard Avenue, Los Angeles, CA 90095-1567 United States
AB: For 10 days surrounding solar conjunction beginning June 16, 2002, the Deep Space Network's experimental antenna in Goldstone took Faraday rotation measurements of Cassini's radio signal. Faraday rotation is the integrated product of the electron density of the corona and the component of the magnetic field parallel to the line of sight. The line of sight of Cassini passed within 1 solar radii of the surface of the sun. Equipped with X- and Ka-band (8 and 32 GHz) capabilities, the signal of Cassini measured the Faraday rotation of the corona through the region of closest approach, 2 coronal mass ejections, and 1 magnetic transient event. Here we present the calculated coronal magnetic fields from the 2002 Faraday rotation experiment.
DE: 7509 Corona
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting