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Title:
Modeling line profile variations of sigma Ori E and theta 1 Ori C
Authors:
Reiners, A.; Stahl, O.; Wolf, B.; Kaufer, A.; Rivinius, T.
Affiliation:
AA(Landessternwarte Heidelberg, Königstuhl, 69117 Heidelberg, Germany ), AB(Landessternwarte Heidelberg, Königstuhl, 69117 Heidelberg, Germany ), AC(Landessternwarte Heidelberg, Königstuhl, 69117 Heidelberg, Germany ), AD(European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany), AE(European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany)
Publication:
Astronomy and Astrophysics, v.363, p.585-592 (2000) (A&A Homepage)
Publication Date:
11/2000
Origin:
A&A
A&A Keywords:
STARS: CHEMICALLY PECULIAR, STARS: EARLY-TYPE, STARS: INDIVIDUAL: SIGMA ORI E, STARS: INDIVIDUAL: THETA 1</SUP&gt, ORI C, STARS: MAGNETIC FIELDS, STARS: STATISTICS
Bibliographic Code:
2000A&A...363..585R

Abstract

We analyse phase-dependent variations of the photospheric lines of the magnetic B star sigma Ori E and the suspected magnetic O star theta 1 Ori C. In the framework of the oblique magnetic rotator model, the observations are interpreted as the result of inhomogeneous chemical abundances - spots - at the stellar surface. This model can at least qualitatively explain the line profile variations with two spots at the magnetic poles of both stars. In the case of sigma Ori E, we find the spots to be overabundant in He and depleted in metals. For theta 1 Ori C the presumed spots would be depleted both in He and in metals. For theta 1 Ori C we also discuss an alternative model with spots of enhanced abundances at the magnetic equator. This model better fits the observations. Chemical fractionation is not expected for theta 1 Ori C and the absorption lines show indications of circumstellar absorption. Therefore, the most likely interpretation of the variations observed in the absorption lines of this star is the presence of excess absorption in a circumstellar cloud and not that of a difference in chemical abundance.

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