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Zeeman Doppler Imaging

Published online by Cambridge University Press:  12 April 2016

William Wehlau  and
John Rice
William Wehlau
Affiliation:
Department of Astronomy, University of Western Ontario London, Ontario N0M 1Z0, Canada
John Rice
Affiliation:
Department of Physics and Astronomy, Brandon University Brandon, Manitoba R7A 6A9, Canada

Abstract

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The mapping of stellar surfaces using the observed profiles of spectral lines is described. The problem is expressed in terms of an integral equation to be solved, using Tikhonov’s method. The local line profiles may be given either by an analytic approximation or by the solution of the equation of transfer with a model atmosphere. The model atmospheres commonly used may not correctly represent the stellar atmosphere which may lead to errors in the derived surface maps. Tests of mapping programs and applications to real stars show the capabilities and limitations of surface mapping. Mapping stellar magnetic fields places more severe demands on the data and computational programs than mapping the abundance distributions.

Type
II. Magnetic Fields: Observations and Theories
Information
International Astronomical Union Colloquium , Volume 138: Peculiar versus Normal Phenomena in A-Type and Related Stars , 1993 , pp. 247 - 257
Copyright
Copyright © Astronomical Society of the Pacific 1993

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