Derivation of the Magnetic Field Configuration above a Solar Active Region using Spatio-spectral Radio Data from the OVSA

Details Derivation of the Magnetic Field Configuration above a Solar Active Region using Spatio-spectral Radio Data from the OVSA Derivation of the Magnetic Field Configuration above a Solar Active Region using Spatio-spectral Radio Data from the OVSA

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.2903t&link_type=abstract

American Astronomical Society, SPD meeting #40, #29.03; Bulletin of the American Astronomical Society, Vol. 41, p.863

Astronomy and Astrophysics

Astronomy

Scientific paper

We present an analysis of multi-frequency radio imaging data derived from observations of AR 10923 taken with the Owens Valley Solar Array on November 10, 2006. This region was chosen because its relative simplicity (alpha configuration) and medium-large size (450 millionths) sunspot may simplify the analysis. The observations span 22 frequencies from 1.4 to 10.6 GHz range. Joint VLA observations were used to increase the spectral resolution of the data, and to provide a means of cross-calibration for the OVSA data. The spectral shapes derived from the brightness temperature maps were used to (1) directly determine the magnetic field at the highest optically thick gyroresonance layer when possible, and (2) an upper bound for it when the spectrum was dominated by free-free emission. Values for the electron temperature and the column emission measure were also derived from the radio spectra. Comparisons of the radio maps with EUV observations from SOHO/EIT were then used to relate the various temperatures and determine a plausible model of the electron density and magnetic field configurations above this active region. The magnetic field model is compared to force-free field extrapolations made from co-temporal Hinode SOT-SP observations of this active region. The differences and similarities are used to asses the validity of the method and magnetic field deduced from OVSA data, which initially has few data points from which to extrapolate the overall magnetic field.

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