Hostname: page-component-77c89778f8-swr86 Total loading time: 0 Render date: 2024-07-19T22:27:42.199Z Has data issue: false hasContentIssue false
  • English
  • Français

Significance of Time Variations in the Be Phenomenon

Published online by Cambridge University Press:  12 April 2016

D. Nelson Limber
D. Nelson Limber*
Affiliation:
University of Virginia, Charlottesville, Va., U.S.A.

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.

When I prepared the discussion in the subsequent sections I did not realize just how subject to question were certain basic ideas relating to the interpretation of the Be phenomenon. In view of the points already raised in the course of this Colloquium, I should like to preface my prepared remarks with certain additional ones.

There appears to be little question that the Be phenomenon has important things to tell us of stellar rotation. It appears almost equally clear that too superficial an approach could well lead to invalid conclusions at any one of a number of points. Some caution therefore, appears advisable. Nevertheless, there appear to be a number of reasons for believing that a relatively simple rotational interpretation of the phenomenon rests on much more solid ground than does any other yet put forward.

Type
Part III / Stellar Rotation in Binaries, Clusters, and Special Objects. Statistics of Stellar Rotation
Information
International Astronomical Union Colloquium , Volume 4: Stellar Rotation , 1970 , pp. 274 - 282
Copyright
Copyright © Reidel 1970

References

Crampin, J. and Hoyle, F.: 1960, Monthly Notices Roy. Astron. Soc. 120, 33.CrossRefGoogle Scholar
Doazan, V.: 1965, Ann. Astrophys. 28, 1.Google Scholar
Hutchings, J. B.: 1967, Observatory 87, 289.Google Scholar
Lacoarret, M.: 1965, Ann. Astrophys. 28, 321.CrossRefGoogle Scholar
Limber, D. N.: 1969, Astrophys. J. 157, 785.Google Scholar
Limber, D. N. and Marlborough, J. M.: 1968, Astrophys. J. 152, 181.Google Scholar
McLaughlin, D. B.: 1961, J. Roy. Astron. Soc. Can. 55, 73.Google Scholar
McLaughlin, D. B.: 1962, Astrophys. J. Suppl. 7, 65.Google Scholar
Sackmann, I. J.: 1968, The Structure and Evolution of Rapidly Rotating B-Type Stars, University of Toronto Thesis.Google Scholar