Features of the Structure of Coronal Magnetic Field on Multifrequency Microwave Observations of Active Regions on the Sun

Details Features of the Structure of Coronal Magnetic Field on Multifrequency Microwave Observations of Active Regions on the Sun Features of the Structure of Coronal Magnetic Field on Multifrequency Microwave Observations of Active Regions on the Sun

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008espm...12.2.89k&link_type=abstract

"12th European Solar Physics Meeting, Freiburg, Germany, held September, 8-12, 2008. Online at http://espm.kis.uni-freiburg.de/,

Physics

Scientific paper

Multiwave observations of active region polarization emission made with the RATAN-600 radio telescope at microwaves, can be effective tools for the study of magnetic field distribution with coronal height for such objects. In the case the projection method is used for determination of the coronal heights of magnetic field. The accuracy of the method is specified by high precision coordinate measurements, which achieved in optical satellite measurements (MDI SOHO) and in transit radio telescope measurements (at RATAN-600). The last conducts the radio observations of polarization emission at many wavelengths in a wide range simultaneously. The developed technique is used to study height magnetic field structure for active regions, which are stable during 2 or 3 days. For measurements of the magnetic field strengths at coronal heights the cyclotron theory is used for many frequencies. It is discovered that magnetic fields with strength about 1000 Gauss reach the heights of the solar atmosphere from 10 to 40 Mm. This is in agreement with observations of magnetic loops in ultraviolet and coincides with the earlier magnetic field measurements of radio astronomy at the level of corona-chromosphere transition level.

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