MHD Modeling of Coronal Mass Ejections: A "Simple" Event

Details MHD Modeling of Coronal Mass Ejections: A "Simple" Event MHD Modeling of Coronal Mass Ejections: A "Simple" Event

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.2202l&link_type=abstract

American Astronomical Society, SPD meeting #37, #22.02; Bulletin of the American Astronomical Society, Vol. 38, p.249

Astronomy and Astrophysics

Astronomy

Scientific paper

In previous work we demonstrated a fast ( 1000 km/s) eruption in an idealized model of the Sun's magnetic field around the time of the May 12, 1997 CME. The model, motivated by an MDI synoptic magnetic field map, contained the sum of a localized bipole (representing an active region) and a large scale axisymmetric magnetic field of dipolar character. Using a zero-beta MHD model, we studied the energization of this magnetic field by shearing flows in the photosphere, as well as an eruption initiated by flux cancellation. While this simple model captured the essence of the magnetic field structure, it limited our ability to compare with CME observations. We will present an improved model that has a more realistic magnetic field distribution, and we will consider the effect of the solar wind on the magnetic field structure and eruption.Research supported by NASA and the Center for Integrated Space Weather Modeling (an NSF Science and Technology Center).

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