HR: 1330h
AN: SH13A-10 [Abstracts]
TI: Comparison of Photospheric Footpoints of Open Magnetic Field Regions using CSSS and PFSS models
AU: * Poduval, B
EM: bala@quake.stanford.edu
AF: Stanford University, 445 Via Palou
HEPL Annex
Stanford University, Stanford, CA 94305 United States
AU: Hoeksema, T
EM: todd@quake.Stanford.edu
AF: Stanford University, 445 Via Palou
HEPL Annex
Stanford University, Stanford, CA 94305 United States
AU: Zhao, X
EM: zhao@quake.stanford.edu
AF: Stanford University, 445 Via Palou
HEPL Annex
Stanford University, Stanford, CA 94305 United States
AB:
Comparison of Photospheric Footpoints of Open Magnetic Field Regions using CSSS and PFSS models The Current--Sheet Source Surface (CSSS) model developed by Zhao and
Hoeksema (1995) assumes a cusp surface at the cusp point of coronal
streamers at around 2.5 Rsun, which divides the corona into
three regions, one bounded by the photosphere and the cusp surface,
the second, between the cusp surface and the source surface, and the
third, the region beyond the source surface. In this model the source surface can be placed closer to the Alfven critical
point which is a great advantage over the traditional Potential Field Source Surface (PFSS) models, where it is at 2.5
Rsun. The source surface magnetic field obtained by CSSS model exhibits little latitudinal variation, which is
consistent with the Ulysses observation of the interplanetary magnetic field (IMF). On the other hand, the source surface
field computed using the PFSS model shows a latitudinal structure. We have carried out a comparative study of the
photospheric footpoints of open magnetic fields obtained dusing the two models. The magnetic neutral line was found to be
coinciding in the two models, as expected. There are significant differences in the locations and sizes of the open field
regions on the photosphere, and they are not always consistent with the observations of coronal holes. We present the results of the comparison.
DE: 2169 Sources of the solar wind
DE: 7509 Corona
DE: 7511 Coronal holes
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly