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Spectrally and spatially resolved Hα emission from Be stars: their disks rotate Keplerian

Published online by Cambridge University Press:  12 July 2011

René D. Oudmaijer ,
Hugh E. Wheelwright ,
Alex C. Carciofi ,
Jon E. Bjorkman  and
Karen S. Bjorkman
René D. Oudmaijer
Affiliation:
School of Physics & Astronomy, University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
Hugh E. Wheelwright
Affiliation:
School of Physics & Astronomy, University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
Alex C. Carciofi
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Rua o Matão 1226, Cidade Universitária, São Paulo, SP 05508-900, Brazil
Jon E. Bjorkman
Affiliation:
Department of Physics & Astronomy, University of Toledo, MS111 2801 W. Bancroft Street, Toledo, OH 43606, USA
Karen S. Bjorkman
Affiliation:
Department of Physics & Astronomy, University of Toledo, MS111 2801 W. Bancroft Street, Toledo, OH 43606, USA
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Abstract

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We test whether Be star disks rotate in a Keplerian or an Angular Momentum Conserving fashion. This is done by employing sub-milli arcsecond spectroastrometry around Hα. We spatially resolve the disks, and are the first to do so at such a high spectral resolution. We fit the emission line profiles with parametric models. The Keplerian models reproduce the spectro-astrometry, whereas the AMC models do not, thereby supporting the viscous disk model for Be stars.

Keywords

line: profilestechniques: high angular resolutionstars: emission-lineBe
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. 418 - 419
Copyright
Copyright © International Astronomical Union 2011

References

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