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Coronal Magnetic Fields Deduced from Radio Methods

Published online by Cambridge University Press:  12 April 2016

A. Krüger and
J. Hildebrandt
A. Krüger
Affiliation:
Astrophysical Institute Potsdam, An der Sternwarte 16, D-O-1591 Potsdam-Babelsberg, Germany
J. Hildebrandt
Affiliation:
Astrophysical Institute Potsdam, An der Sternwarte 16, D-O-1591 Potsdam-Babelsberg, Germany

Abstract

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Major problems of the physics of the solar atmosphere and processes of solar activity are due to the poor knowledge of the magnetic fields outside the photosphere. Unique methods to determine magnetic fields in the corona and chromosphere make use of radio observations in close connection with information obtained in other spectral ranges e.g. the optical and X-ray regions. Based on relevant emission and propagation processes, the basic radio methods providing information on the parent magnetic fields are summarized. Signatures in the microwave and meter wave regions are used to derive magnetic field parameters at different levels in the solar atmosphere of active regions during quiet and flaring conditions. Implications on fine and gross structures are briefly discussed and consequences on acting physical processes mentioned.

Information

Type
Session 5. Fields in the Chromosphere and Corona
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993, pp. 249 - 257
Copyright
Copyright © Astronomical Society of the Pacific 1993

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