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Title:
Be-star rotation: how close to critical?
Authors:
Townsend, R. H. D.; Owocki, S. P.; Howarth, I. D.
Affiliation:
AA(Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT; Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), AB(Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT; Bartol Research Institute, University of Delaware, Newark, DE 19716, USA), AC(Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 350, Issue 1, pp. 189-195. (MNRAS Homepage)
Publication Date:
05/2004
Origin:
MNRAS
MNRAS Keywords:
line: profiles, techniques: spectroscopic, stars: emission-line, Be, stars: fundamental parameters, stars: rotation
DOI:
10.1111/j.1365-2966.2004.07627.x
Bibliographic Code:
2004MNRAS.350..189T

Abstract

We argue that, in general, observational studies of Be-star rotation have paid insufficient attention to the effects of equatorial gravity darkening. We present new line-profile calculations that emphasize the insensitivity of line width to rotation for fast rotators. Coupled with a critical review of observational procedures, these calculations suggest that the observational parameter v sini may systematically underestimate the true projected equatorial rotation velocity, ve sini, by some tens of per cent for rapid rotators. A crucial implication of this work is that Be stars may be rotating much closer to their critical velocities than is generally supposed, bringing a range of new processes into contention for the elusive physical mechanism responsible for the circumstellar disc thought to be central to the Be phenomenon.

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