Computer Science – Sound
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh52a..06j&link_type=abstract
American Geophysical Union, Spring Meeting 2004, abstract #SH52A-06
Computer Science
Sound
2164 Solar Wind Plasma, 6969 Remote Sensing, 6979 Space And Satellite Communication, 7513 Coronal Mass Ejections, 7531 Prominence Eruptions
Scientific paper
The Cassini Solar Faraday Rotation Experiment was conducted during the spacecraft's solar conjunctions in 2002 and 2003. A total of 160 hours of open-loop radio science data was collected at frequencies of 8 and 32 GHz (X- and Ka-bands), i.e., frequencies much higher than the plasma frequencies, but sufficiently low to undergo measurable Faraday rotation in the solar corona. During the 2002 experiment, four Coronal Mass Ejections crossed the signal ray path between Cassini and the Earth, each one imparting a different signature in the radio sounding data. The first occurred during the day of conjunction when the spacecraft's signal ray path passed to within approximately 2 solar radii of the Sun's center. The second occurred 1 day later at a solar offset distance of 3 solar radii. As shown by the EIT imager on SOHO, this event was oriented almost perpendicular to the first CME. It had a significant impact on the signal, causing the Ka-band translator on Cassini to lose lock on the uplink signal from Earth. The 3rd and 4th CMEs occurred 2 days later as a paired event when the Cassini solar offset was roughly 5 solar radii. The data received during the minimum solar elongation attained during the 2003 conjunction (proximate ray path point: 1.25 solar radii) were highly variable and represent the closest radio occultation measurement to the surface of the Sun. We discuss the Cassini Faraday Rotation data and develop models of the coronal electron density and magnetic field to simulate the measurements.
Anderson John D.
Asmar Sami W.
Bird Michael K.
Jensen Elizabeth A.
Russell Christopher T.
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