Hostname: page-component-6bf8c574d5-nvqbz Total loading time: 0 Render date: 2025-03-08T07:26:36.296Z Has data issue: false hasContentIssue false
  • English
  • Français

The stability of massive stars

Published online by Cambridge University Press:  26 May 2016

W. Glatzel ,
M. Kiriakidis  and
K.J. Fricke
W. Glatzel
Affiliation:
Universitäts-Sternwarte, Geismarlandstr. 11, D-37083 Göttingen, FRG
M. Kiriakidis
Affiliation:
Universitäts-Sternwarte, Geismarlandstr. 11, D-37083 Göttingen, FRG
K.J. Fricke
Affiliation:
Universitäts-Sternwarte, Geismarlandstr. 11, D-37083 Göttingen, FRG

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.

An investigation of the stability properties of stellar models describing massive stars is motivated observationally by the necessity to explain the observed Humphreys - Davidson (HD) limit and the variability of the most massive stars known, i.e. the existence of luminous blue variables (LBVs). Theoretically, a determination of the upper mass limit for stable stellar objects together with its physical explanation and interpretation is of fundamental interest.

Type
1. Pulsation and Rotation
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 73 - 74
Copyright
Copyright © Kluwer 1994 

References

Glatzel, W., Kiriakidis, M.: 1993, MNRAS 263, 375 CrossRefGoogle Scholar
Kiriakidis, M., Fricke, K.J., Glatzel, W.: 1993, MNRAS 264, 50 CrossRefGoogle Scholar
Stothers, R.B., Chin, C.: 1993, ApJ 408, L85 Google Scholar