MHD Modeling of the May 12, 1997 CME

Details MHD Modeling of the May 12, 1997 CME MHD Modeling of the May 12, 1997 CME

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh13a0283l&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH13A-0283

Physics

7509 Corona, 7524 Magnetic Fields, 7827 Kinetic And Mhd Theory

Scientific paper

In previous work we constructed an idealized model of the coronal magnetic field on May 11, 1997, preceding the CME that occurred on the following day. 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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