HR: 1340h
AN: SH13A-1157    [Abstracts]
TI: MHD Modeling of Differential Rotation
AU: * Lionello, R
EM: lionellor@saic.com
AF: Science Applications International Corporation, 10260 Campus Point Dr., San Diego, CA 92121-1578 United States
AU: Linker, J A
EM: linkerj@saic.com
AF: Science Applications International Corporation, 10260 Campus Point Dr., San Diego, CA 92121-1578 United States
AU: Miki\'c, Z
EM: mikicz@saic.om
AF: Science Applications International Corporation, 10260 Campus Point Dr., San Diego, CA 92121-1578 United States
AU: Riley, P
EM: rileype@saic.com
AF: Science Applications International Corporation, 10260 Campus Point Dr., San Diego, CA 92121-1578 United States
AB: In the Fisk model differential rotation on the solar photosphere is thought to cause large excursions of magnetic field lines in the upper corona and in the heliosphere. This is in contrast with the apparently rigid rotation of some coronal holes. The model of Fisk et al.\ (1999) consists of a dipole field with the magnetic axis distinct from the rotation axis. The field from the northern and southern polar holes superexpands into the solar wind. In order to reconcile the pattern of velocity in the upper corona with the photospheric differential flow, magnetic reconnection is invoked between open field lines and low-lying loops. This mechanism releases the plasma trapped in the closed field lines into the corona and originates the slow solar wind. We have used our MHD model in spherical coordinates to study this mechanism. We have imposed a magnetic flux distribution as in Fisk et al.\ (1999). After relaxing the system to steady state, we have applied differential rotation for the equivalent of 5 rotations. We will describe the changes in the coronal magnetic field in response to the photospheric flows.
DE: 7509 Corona
DE: 7511 Coronal holes
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting