Coronal Magnetic Fields from Microwave Polarization Observations

Details Coronal Magnetic Fields from Microwave Polarization Observations Coronal Magnetic Fields from Microwave Polarization Observations

Aug 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996soph..167..167a&link_type=abstract

Solar Physics, Volume 167, Issue 1-2, pp. 167-179

Physics

14

Scientific paper

The solar active region (AR) 7530 was observed at 6 cm on July 3 and 4, 1993 with the Westerbork Synthesis Radio Telescope, using a multi-channel receiver with very narrow bandwidth. We compare the radio data with Yohkoh SXT observations and with the magnetic field extrapolated from the Marshall vector magnetograms in the force-free and current-free approximations. The comparison with soft X-rays shows that, although a general agreement exists between the shape of the radio intensity map and the X-ray loops, the brightness temperature, T b, obtained using the parameters derived from the SXT is much lower than that observed. The comparison with the extrapolated photospheric fields shows instead that they account very well for the observed T b above the main sunspots, if gyroresonance emission is assumed. In the observation of July 4 an inversion and strong suppression of the circular polarization was clearly present above different portions of the AR, which indicates that particular relationships exist between the electron density and the magnetic field in the region where the corresponding lines of sight cross the field quasi-perpendicularly. The extrapolated magnetic field at a much higher level (˜ 1010 cm), satisfies the constraints required by the wave propagation theory all over the AR. However, a rather low electron density is derived.

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