Magnetohydrodynamic Simulations of Plumes in the Solar Wind.

Details Magnetohydrodynamic Simulations of Plumes in the Solar Wind. Magnetohydrodynamic Simulations of Plumes in the Solar Wind.

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.1408l&link_type=abstract

American Astronomical Society, SPD meeting #40, #14.08; Bulletin of the American Astronomical Society, Vol. 41, p.834

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Coronal plumes are raylike structures that are seen extending for many solar radii above the limb of the Sun in white light observations. They are associated with localized areas of mixed-polarity photospheric magnetic field within the predominantly unipolar coronal holes and play an important role in the origin of the fast solar wind. In the past, the expansion of plumes into the heliosphere has been studied extensively with pressure balanced models. We have used our computational MHD code that includes thermal conduction, radiation losses, and coronal heating to study self-consistently the dynamics of plumes in the solar wind. To generate the plumes, we have prescribed heating functions exponentially decreasing in radius as in Wang (1990). Funding provided by NASA Solar and Heliospheric Physics Program.

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