Coronal Loop Recognition: A Diagnostic Tool for Magnetic Field Extrapolation Models

Details Coronal Loop Recognition: A Diagnostic Tool for Magnetic Field Extrapolation Models Coronal Loop Recognition: A Diagnostic Tool for Magnetic Field Extrapolation Models

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.1604s&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #16.04; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

Scientific paper

Constraining the structure and extent of the coronal magnetic field is important for theories of coronal heating. This can be accomplished by matching the models of magnetic fields derived by extrapolating measurements of surface magnetic flux, with highly detailed structure present in EUV and X-ray images of the corona. Using high resolution TRACE images we detect loops in an automated manner, and aim to replace the currently used method of manually selecting pixels that might comprisea loop. We apply this method to a set of TRACE images and identify loops for further analysis. We fit force-free potential field models of the magnetic field to these loops and derive useful parameters that describe the geometric and physical parameters of the loop. We find that the loops are generally of length > 1010 cm. If assumed to be in static equilibrium, the loop top temperatures are 3-5 MK. the field lines are characterized by strength ranging from 0.4-27 G. After carrying out numerous Monte Carlo simulations, each time varying different parameters used in the program, we found this new automated process to be stable and robust. We thank the Harvard-Smithsonian Summer REU program for making this summer project possible as well as a grant from NASA (NASA grant NNG05GM44G), and the NSF for funding the REU program.

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