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Temperature, Abundance and Magnetic Mapping of Stellar Atmospheres

Published online by Cambridge University Press:  12 April 2016

J.-F. Donati
J.-F. Donati*
Affiliation:
University of Western Ontario, London Ontario, N6A 3K7Canada

Abstract

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In this paper, I review recent progress in the domain of indirect imaging of stellar atmospheres. Since all stars other than the Sun are too far away for us to disclose any feature on their surface directly, one has to use an indirect tool to image their atmosphere. This method (Doppler Imaging) takes advantage of a star’s rotation to identify and characterise inhomogeneities on its surface. This is done by studying both how inhomogeneities (carried in and out of the observer’s view by rotation) modulate photometric and spectroscopic data with time, and how surface features distort the shape of line profiles at a given rotational phase. In the last decade, Doppler Imaging has first been applied to abundance mapping of magnetic Ap stars, then extended to temperature and magnetic mapping of cool active stars. Allowing a solar-like way of studying the surface of stars, this technique provides a wealth of information about stellar atmospheres and, in particular, about the physical processes which dictate their dynamics and energy balance.

Type
II. Atmospheres, a window to the interior
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 136 - 149
Copyright
Copyright © Astronomical Society of the Pacific 1993

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