Heliospheric energetic particle observations by the Cassini spacecraft

Details Heliospheric energetic particle observations by the Cassini spacecraft Heliospheric energetic particle observations by the Cassini spacecraft

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja....11131l&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #11131

Computer Science

Scientific paper

We present a preliminary analysis of the energetic particle observations performed by the Cassini spacecraft during its heliospheric cruise to Saturn. This period covers three years (2000-2002) of maximum activity in the present solar cycle. Energetic particle intensity enhancements observed by Cassini during this period are associated with either Solar Energetic Particle (SEP) events or Corotating Interaction Regions (CIRs). The fleet of spacecraft present in the inner heliosphere (<10 AU) during this period allows the comparison of SEP events and CIR events at several heliospheric locations and under different interplanetary conditions. We discuss the characteristics of the largest SEP events observed by Cassini, and simultaneously by ACE and Ulysses, in terms of both the locations of the spacecraft, the properties of the parent solar events and the interplanetary conditions for particle transport between the Sun and each spacecraft. Cassini observations at ˜6-7 AU and in the ecliptic plane show that whereas high-energy (>10 MeV) proton intensities are dominated by the favorable magnetic connection between the spacecraft and the solar source of particles, the largest low-energy (<5 MeV) proton intensities are associated with the passage of CME-driven interplanetary shocks. In contrast to 1 AU observations, near-relativistic (˜100 keV) electrons also attain their highest intensities at the passage of interplanetary shocks.

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