34th Solar Physics Division Meeting, June 2003
Session 4 Corona II
Poster, Monday, June 16, 2003, 3:30-5:00pm, Mezzanine

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[4.17] Numerical simulation of a quadrupolar magnetic field in the corona

T. Magara, D. W. Longcope (Montana State University)

We carried out ideal, compressible MHD numerical simulations of a coronal magnetic field that evolves in response to the motion imposed at the photospheric boundary. The magnetic field is formed above a quadrupolar region in the photosphere which is composed of two dipoles each centered at the origin. Starting from a potential field that forms four magnetic flux domains in the corona, the magnetic field develops when a rotational motion is imposed to the inner dipole (the outer dipole is fixed during the simulation). We discuss the evolution of each magnetic flux domain as well as the temporal deveopment of current flowing in those flux domains. We also show the time variaiton of the free magnetic energy and magnetic helicity accumulated in the corona, both of which are used to diagnose the coronal field.

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Bulletin of the American Astronomical Society, 35 #3
© 2003. The American Astronomical Soceity.