HR: 1340h
AN: SH13A-1153 [Abstracts]
TI: A Comparison of Coronal Magnetic Field and Heliospheric Current Sheet Derived From the MAS and WSA
Models
AU: * McGregor, S L
EM: slmic@bu.edu
AF: Boston University, Department of Astronomy
725 Commonwealth Ave, Boston, MA 02215
United States
AU: Hughes, W J
EM: hughes@bu.edu
AF: Boston University, Department of Astronomy
725 Commonwealth Ave, Boston, MA 02215
United States
AU: Arge, C N
EM: Nick.Arge@hanscom.af.mil
AF: Air Force Research Laboratory, Space Vehicles Directorate
29 Randolf Road, Hanscom AFB, MA 01731
United States
AU: Riley, P
EM: pete@peteriley.org
AF: SAIC, 10260 Campus Point Drive, San Diego, CA 92121
United States
AU: Linker, J
EM: JON.A.LINKER@saic.com
AF: SAIC, 10260 Campus Point Drive, San Diego, CA 92121
United States
AB:
The coronal magnetic field is exceptionally complex and exceedingly difficult to measure. Several models have been put forth
which generate solutions for the coronal fields based on photospheric field measurements. Here we examine and compare the
underlying structures and topologies of the solar coronal magnetic field and the heliospheric current sheet derived from two
very different coronal models, SAIC's MAS model and the coupled potential field source surface+Schatten current sheet
(PFSS+SCS) model used in the Wang-Sheeley-Arge (WSA) model. The MAS model solves the three-dimensional resistive MHD
equations using a semi-implicit finite difference scheme utilizing staggered meshes. The WSA model uses the values at the
outer boundary or "source surface" (R=2.5Rs) as the input for the SCS model. The same synoptic maps derived from the
line-of-sight photospheric magnetic field for selected rotations during solar minimum and solar maximum periods of the solar
cycle are used as the boundary conditions for both models. We compare the two magnetic field solutions along with the shape
and size of the two regions of open solar magnetic field lines and the total open flux. We also compare the location and
shape of the inner heliospheric current sheet obtained by the two models.
DE: 7509 Corona
DE: 7511 Coronal holes
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting