Hostname: page-component-848d4c4894-nmvwc Total loading time: 0 Render date: 2024-07-05T20:30:49.188Z Has data issue: false hasContentIssue false
  • English
  • Français

A survey of line profile variations in non-emission line B0–B5 III–V stars

Published online by Cambridge University Press:  26 May 2016

M. S. Fieldus  and
C. T. Bolton
M. S. Fieldus
Affiliation:
David Dunlap Observatory, University of Toronto Richmond Hill, Ontario, L4C 4Y6, CANADA
C. T. Bolton
Affiliation:
David Dunlap Observatory, University of Toronto Richmond Hill, Ontario, L4C 4Y6, CANADA

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Some investigators have attributed the photometric and spectral line profile variations (lpv) that are common among the B stars to nonradial pulsation while others have attempted to explain them by rotation of photospheric or circumstellar structures with respect to our line of sight. One of the problems in resolving this debate has been our lack of knowledge of how these variations depend on fundamental stellar characteristics. Surveys of lpv have covered the Be and a few Bn stars (D. Penrod, unpublished), the O stars (Fullerton 1990), and B8-B9.5 main sequence stars (Baade 1989), but noone has carried out a systematic search for lpv among the near main sequence, non-emission line early- and mid-B stars. This paper describes preliminary results from such a survey.

Type
1. Pulsation and Rotation
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 108 - 109
Copyright
Copyright © Kluwer 1994 

References

Baade, D.: 1989, A. & A. 222, 200 Google Scholar
Fullerton, A.: 1991, Ph.D. thesis University of Toronto,Google Scholar
Smith, M. A.: 1977, Ap.J. 215, 574 Google Scholar
Smith, M. A.: 1978, Ap.J. 224, 927 Google Scholar