The altitude structure of the coronal magnetic field of AR 10933

The magnetic fields of solar active regions are analyzed using a method based on comparing the spatial structures of the reconstructed magnetic field and of the radio emission of the active region. Two approaches are used: comparing the radio size of the active region and the corresponding size calc...

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Bibliographic Details
Published in:Astronomy reports 2012-10, Vol.56 (10), p.790-799
Main Authors: Kaltman, T. I., Bogod, V. M., Stupishin, A. G., Yasnov, L. V.
Format: Article
Language:English
Subjects:
Altitude
Astronomy
Corona
Electron density
Emittance
Magnetic fields
Mathematical analysis
Observations and Techniques
Physics
Physics and Astronomy
Radio emission
Solar flares
Spectral emittance
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Summary:The magnetic fields of solar active regions are analyzed using a method based on comparing the spatial structures of the reconstructed magnetic field and of the radio emission of the active region. Two approaches are used: comparing the radio size of the active region and the corresponding size calculated using the reconstructed magnetic field, and comparing the radio spectra that are observed and calculated using the reconstructed magnetic field. Overall, the calculated sizes and spectra correspond fairly well to the observational data, making it possible to estimate physical parameters of the emitting region, such as the electron density and temperature.
ISSN:1063-7729
1562-6881
DOI:10.1134/S1063772912100022