A Comparison of Coronal Magnetic Field and Heliospheric Current Sheet Derived From the MAS and WSA Models

Details A Comparison of Coronal Magnetic Field and Heliospheric Current Sheet Derived From the MAS and WSA Models A Comparison of Coronal Magnetic Field and Heliospheric Current Sheet Derived From the MAS and WSA Models

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsh13a1153m&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SH13A-1153

Physics

7509 Corona, 7511 Coronal Holes, 7524 Magnetic Fields

Scientific paper

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.

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