Townsend, RHD;
Owocki, SP;
Howarth, ID;
(2004)
Be-star rotation: how close to critical?
MON NOT R ASTRON SOC
, 350
(1)
189 - 195.
10.1111/j.1365-2966.2004.07627.x.
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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 newline-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 sin i may systematically underestimate the true projected equatorial rotation velocity, v e sin i, 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.
| Type: | Article |
|---|---|
| Title: | Be-star rotation: how close to critical? |
| Open access status: | An open access version is available from UCL Discovery |
| DOI: | 10.1111/j.1365-2966.2004.07627.x |
| Keywords: | line : profiles, techniques : spectroscopic, stars : emission-line, Be, stars : fundamental parameters, stars : rotation, MAIN-SEQUENCE STARS, BLANKETED MODEL ATMOSPHERES, V-SIN-I, SPECTRAL CLASSIFICATION, VELOCITY DETERMINATIONS, STELLAR ATMOSPHERES, OPACITY MECHANISM, LINE-PROFILES, SHELL STARS, EMISSION |
| UCL classification: | UCL UCL > Provost and Vice Provost Offices > UCL BEAMS UCL > Provost and Vice Provost Offices > UCL BEAMS > Faculty of Maths and Physical Sciences UCL > Provost and Vice Provost Offices > UCL BEAMS > Faculty of Maths and Physical Sciences > Dept of Physics and Astronomy |
| URI: | https://discovery.ucl.ac.uk/id/eprint/9630 |
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