Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh51b..01b&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SH51B-01
Astronomy and Astrophysics
Astrophysics
7500 Solar Physics, Astrophysics, And Astronomy, 7509 Corona, 7511 Coronal Holes, 7524 Magnetic Fields, 7529 Photosphere
Scientific paper
Traditionally, Potential Field Source Surface (PFSS) models have used low-degree spherical harmonic transforms to calculate magnetic fields and estimate the large-scale coronal structure. This has been for two reasons; first, low-resolution data restricted the maximum degree of the transforms and second, the global magnetic structures of interest only required a low-degree expansion due to their distance from the photosphere. One of the most important applications of PFSS models has been to determine where open coronal field lines intersect the photosphere. However, the magnetic field near the solar surface is far more structured than can be accurately described by low-degree models. The combination of PFSS models capable of high-degree transforms and data from high-resolution solar imaging facilities is required to accurately determine the photospheric foot-point locations of coronal field lines. We present preliminary results from a new PFSS model that is capable of matching the spatial resolution of the MDI synoptic magnetograms used as input. We compare results to lower-degree models, and show how variations in the maximum spherical harmonic degree (l>1000) affect field line locations at the photosphere. We also discuss the computational difficulties inherent in these calculations.
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