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Magnetic Doppler imaging of early-type stars

Published online by Cambridge University Press:  12 July 2011

Oleg Kochukhov ,
Thomas Rivinius ,
Mary E. Oksala  and
Iosif Romanyuk
Oleg Kochukhov
Affiliation:
Dept. Physics and Astronomy, Uppsala University, Box 516, 75120 Uppsala, Sweden
Thomas Rivinius
Affiliation:
European Southern Observatory, Casilla 19001, Santiago 19, Chile
Mary E. Oksala
Affiliation:
Dept. of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA
Iosif Romanyuk
Affiliation:
Special Astrophysical Observatory of RAS, Nizhnij Arkhyz 369167, Russia
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Abstract

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Doppler imaging of early-type magnetic stars is the most advanced method to interpret their line profile variations. DI allows us to study directly a complex interplay between chemical spots, magnetic fields, and the mass loss. Here we outline the general principles of the surface mapping of stars, discuss adaption of this technique to early-type stars and present several recent examples of the abundance and magnetic mapping performed for rapidly rotating early-B stars. In particular, we present the first Doppler images for the very fast rotating He-rich star HR 7355 and a reconstruction of magnetic field for the well-known Bp star σ Ori E. We also present new magnetic maps for the He-strong star HD 37776, which possesses one of the most complex magnetic field topologies among the upper main sequence stars.

Keywords

polarizationstars: chemically peculiarstars: magnetic fieldsstars: atmospheresstars: individual (HR 7355, σOri E, HD 37776)

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