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The inference of the magnetic field vector in prominences

Published online by Cambridge University Press:  06 January 2014

Bruce W. Lites
Bruce W. Lites*
Affiliation:
High Altitude Observatory, National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO 80307-3000, USA email: lites@ucar.edu
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Abstract

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Prominences owe their existence to the presence of magnetic fields in the solar corona. The magnetic field determines their geometry and is crucial to their stability, energetics, and dynamics. This review summarizes techniques for measurement of the magnetic field vector in prominences. New techniques for inversions of full Stokes spectro-polarimetry, incorporating both the Zeeman and Hanle mechanisms for generation and modification of polarization, are now at the forefront. Also reviewed are measurements of the magnetic fields in the photosphere below prominences, and how they may be used to infer the field geometry in and surrounding the prominence itself.

Keywords

magnetic fieldspolarizationscatteringdata analysispolarimetricSun: prominencesSun: filaments
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S300: Nature of Prominences and their role in Space Weather , June 2013 , pp. 101 - 111
Copyright
Copyright © International Astronomical Union 2013 

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