Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh31b1798p&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH31B-1798
Astronomy and Astrophysics
Astrophysics
[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7511] Solar Physics, Astrophysics, And Astronomy / Coronal Holes, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields, [7529] Solar Physics, Astrophysics, And Astronomy / Photosphere
Scientific paper
The standard method for modeling the global coronal field is to calculate a potential-field source-surface (PFSS) solution based on a photospheric synoptic map, a full-surface map of the photospheric radial field component based on observations taken throughout a solar rotation. At the spherical source surface in the model the field is forced to be radial, modeling the coronal field being forced open by the solar wind. The radius of the source surface is a free parameter. Using synoptic maps from NSO's GONG and SOLIS programs and from Wilcox Solar Observatory for a set of approximately 30 rotations we generate PFSS models and compare them to NASA STEREO observations of coronal holes and streamer structures. The SOLIS maps are constructed converting line-of-sight field measurements to radial field maps in two different ways, (1) a standard diachronic approach where the photospheric field is assumed to be approximately radial, and (2) a synchronic approach that doesn't assume a radial photospheric field. The GONG and Wilcox maps are constructed the first way only. Differences between the modeled and observed coronal structures are calculated quantitatively for each permutation of data source, map construction method and source-surface radius and the implications for synoptic map construction and PFSS modeling are discussed. We also test models based on 5 rotations of GONG zero-point-corrected data.
Bertello Luca
Petrie G. J.
Tran T. T.
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