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On the physical aspects of accretion by stars

Published online by Cambridge University Press:  24 October 2008

F. Hoyle  and
R. A. Lyttleton
F. Hoyle
Affiliation:
St John's CollegeCambridge
R. A. Lyttleton
Affiliation:
St John's CollegeCambridge
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Extract

The presence of H2 molecules reduces the temperature of the cosmical cloud to a value that is small compared with the estimate given by Eddington. The necessary conditions for the molecules to persist at the capture radius of hot stars are investigated in the present paper, and it is shown that provided that the density of the cosmical cloud is sufficiently high the molecules will not suffer appreciable dissociation, and that radiation pressure will have only a negligible effect on the hydrogen. The critical density for a typical B star appears to be about 5 × 10−21 g. per c.c.

Type
Research Article
Information
Mathematical Proceedings of the Cambridge Philosophical Society , Volume 36 , Issue 4 , October 1940 , pp. 424 - 437
Copyright
Copyright © Cambridge Philosophical Society 1940

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References

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