Validation of the 3D MHD Solar Wind Model Results with Voyager and Pioneer Data

Details Validation of the 3D MHD Solar Wind Model Results with Voyager and Pioneer Data Validation of the 3D MHD Solar Wind Model Results with Voyager and Pioneer Data

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsm23a0307l&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SM23A-0307

Other

5734 Magnetic Fields And Magnetism, 5737 Magnetospheres (2756), 7924 Forecasting (2722), 7959 Models, 7974 Solar Effects

Scientific paper

The CISM (Center for Integrated Space Weather Modeling) inner heliospheric model ENLIL together with the Wang-Sheeley-Arge (WSA) coronal magnetic field model 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 ENLIL+WSA 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. We validate this model, newly available at the Community Coordinated Modeling Center (CCMC), using archives of outer heliospheric solar wind measurements from the Pioneer and Voyager spacecrafts. It is known from both Voyager and Cassini that Saturn's magnetosphere responds to solar wind dynamic pressure enhancements. Agreement of the model with observations could suggest 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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