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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

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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