Physics
Scientific paper
Dec 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh11a0250l&link_type=abstract
American Geophysical Union, Fall Meeting 2005, abstract #SH11A-0250
Physics
7509 Corona, 7524 Magnetic Fields
Scientific paper
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 respo nse to the photospheric flows.
Linker Jon A.
Lionello Roberto
Mikic Zoran
Riley Pete
No associations
LandOfFree
MHD Modeling of the Latitudinal Excursion of Magnetic Field Lines in the Solar Corona does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with MHD Modeling of the Latitudinal Excursion of Magnetic Field Lines in the Solar Corona, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and MHD Modeling of the Latitudinal Excursion of Magnetic Field Lines in the Solar Corona will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-755270