Hostname: page-component-745bb68f8f-d8cs5 Total loading time: 0 Render date: 2025-01-13T00:38:24.236Z Has data issue: false hasContentIssue false
  • English
  • Français

Is There Mass Loss in B Canis Majoris Stars?

Published online by Cambridge University Press:  12 April 2016

Janet Rountree Lesh  and
Alan H. Karp
Janet Rountree Lesh
Affiliation:
Laboratory for Astronomy and Solar Physics, Goddard Space Flight Center
Alan H. Karp
Affiliation:
Department of Physics and Astronomy, Dartmouth College

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.

The purpose of this communication is to show that one possible explanation for the asymmetric line profiles observed in β Canis Majoris stars may be the presence of a stellar wind superimposed on a radial or nonradial pulsation.

Type
Part III: Evolved Stars
Information
International Astronomical Union Colloquium , Volume 42: The Interaction of Variable Stars with their Environment , 1977 , pp. 625 - 632
Copyright
Copyright © Veröff. Der Remeis-Sterwarte 1977

References

Huang, S.S., Struve, O. 1955. Ap. J. 122, 103.Google Scholar
Kurucz, R. L., Peytremann, E., Avrett, E. H. 1974. Blanketed Model Atmospheres for Early-Type Stars. Washington, D.C.: Smithsonian Institution.Google Scholar
Laskarides, P. G., Odgers, G. J., Climenhaga, J. L. 1971. A.J. 76, 363.Google Scholar
Osaki, Y. 1971. P.A.S.J. 23, 485.Google Scholar