Solar Wind Modeling of Cassini-Approach Observations

Details Solar Wind Modeling of Cassini-Approach Observations Solar Wind Modeling of Cassini-Approach Observations

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufm.p51a1418l&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #P51A-1418

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6275 Saturn, 2102 Corotating Streams, 2169 Sources Of The Solar Wind

Scientific paper

The CISM (Center for Integrated Space Weather Modeling) inner heliospheric model CORHEL is extended to 10 AU to investigate how well this solar magnetogram-based 3D MHD model describes the solar wind influence on Saturn's magnetosphere. The CORHEL model describes the steady solar wind stream structure and its origins in the corona. It has been tuned to provide a simulation of the solar wind parameters at 1 AU including plasma moments and interplanetary magnetic field magnitude and polarity in the absence of disturbances from coronal transients. Comparisons with the Cassini CAPS plasma and magnetometer field observations during Cassini's approach to Saturn show good agreement with the model, in part because of a low solar activity and a particularly simple and steady interplanetary sector pattern during the months before the Saturn orbit insertion (SOI). It is known that Saturn's magnetosphere responds to solar wind dynamic pressure enhancements, which are evident in this period with striking regularity. The model agreement suggests that a viable option is available both to predict such enhancements from co-rotating stream interaction regions, as well as to provide an approximation to solar wind conditions when Cassini is inside Saturn's magnetosphere. Moreover, as radial alignment with other close-in spacecraft is not required, this study illustrates the potential use of state-of-the-art numerical models to study space weather on a solar-system-wide scale.

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