Hostname: page-component-586b7cd67f-gb8f7 Total loading time: 0 Render date: 2024-11-26T08:28:32.325Z Has data issue: false hasContentIssue false
  • English
  • Français

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
Get access Rights & Permissions [Opens in a new window]

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

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

* Proc. Cambridge Phil. Soc. 35 (1939), 405 and 592.Google Scholar

* Eddington, , Internal constitution of the stars (Cambridge, 1926), p. 376.Google Scholar

† Heitler, , Quantum theory of radiation (Oxford, 1936), p. 172.Google Scholar

* Mott, and Massey, , Theory of atomic collisions (Oxford, 1933), p. 217Google Scholar. Fowler, , Statistical mechanics, 2nd ed. (Cambridge, 1936), p. 93.Google Scholar

† Stückelberg, and Morse, , Phys. Rev. 36 (1930), 16.CrossRefGoogle Scholar

* Heitler, loc. cit. p. 109.

* Stückelberg and Morse, loc. cit. p. 22.

* Struve, and Elvey, , Astrophysical J. 88 (1938), 364CrossRefGoogle Scholar and 89 (1939), 119 and 517.

* ν here is 2π times the frequency, so that the energy is ℏν.

* McKellar, , Publ. Astron. Soc. Pacific, 52 (1930), 187CrossRefGoogle Scholar, and Adams, , Harvard Announcement Card, No. 526Google Scholar. We are indebted to a referee for drawing our attention to these results.

* Astrophysical J. 89 (1939), 526.Google Scholar