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Populations of Be stars: stellar evolution of extreme stars

Published online by Cambridge University Press:  12 July 2011

Christophe Martayan ,
Thomas Rivinius ,
Dietrich Baade ,
Anne-Marie Hubert  and
Jean Zorec
Christophe Martayan
Affiliation:
ESOChile; email: cmartaya@eso.org GEPI-Observatoire de Meudon, France
Thomas Rivinius
Affiliation:
ESOChile; email: cmartaya@eso.org
Dietrich Baade
Affiliation:
ESOGermany
Anne-Marie Hubert
Affiliation:
GEPI-Observatoire de Meudon, France
Jean Zorec
Affiliation:
Institut d'Astrophysique de Paris, France
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Abstract

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Among the emission-line stars, the classical Be stars known for their extreme properties are remarkable. The Be stars are B-type main sequence stars that have displayed at least once in their life emission lines in their spectrum. Beyond this phenomenological approach some progresses were made on the understanding of this class of stars. With high-technology techniques (interferometry, adaptive optics, multi-objects spectroscopy, spectropolarimetry, high-resolution photometry, etc) from different instruments and space mission such as the VLTI, CHARA, FLAMES, ESPADONS-NARVAL, COROT, MOST, SPITZER, etc, some discoveries were performed allowing to constrain the modeling of the Be stars stellar evolution but also their circumstellar decretion disks. In particular, the confrontation between theory and observations about the effects of the stellar formation and evolution on the main sequence, the metallicity, the magnetic fields, the stellar pulsations, the rotational velocity, and the binarity (including the X-rays binaries) on the Be phenomenon appearance is discussed. The disks observations and the efforts made on their modeling is mentioned. As the life of a star does not finish at the end of the main sequence, we also mention their stellar evolution post main sequence including the gamma-ray bursts. Finally, the different new results and remaining questions about the main physical properties of the Be stars are summarized and possible ways of investigations proposed. The recent and future facilities (XSHOOTER, ALMA, E-ELT, TMT, GMT, JWST, GAIA, etc) and their instruments that may help to improve the knowledge of Be stars are also briefly introduced.

Keywords

stars: emission-lineBestars: formationstars: evolutionstars: rotationstars: abundancesstars: magnetic fieldsstars: oscillations (including pulsations)binaries: generalsurveysgamma rays: bursts
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 242 - 253
Copyright
Copyright © International Astronomical Union 2011

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