Hostname: page-component-586b7cd67f-gb8f7 Total loading time: 0 Render date: 2024-11-30T03:48:48.378Z Has data issue: false hasContentIssue false
  • English
  • Français

11. Effective Temperatures of White Dwarfs

Published online by Cambridge University Press:  14 August 2015

J. B. Oke  and
H. L. Shipman
J. B. Oke
Affiliation:
Hale Observatories, California Institute of Technology, Carnegie Institution of Washington
H. L. Shipman
Affiliation:
Hale Observatories, California Institute of Technology, Carnegie Institution of Washington

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.

White dwarf stars are among the most challenging and interesting objects which can be studied. Because they represent the interiors of highly-evolved stars, the chemical composition can be enormously variable from object to object. Furthermore, because of the very large gravities, the composition of the atmosphere may be very different from that in the interior. The theory of the degenerate interior provides a relation among mass, radius and chemical composition. Since temperatures, effective gravities, and redshifts can, for certain stars, provide further relations between mass and radius, one can hope to make checks on the theory which are not possible with ordinary stars.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 42: White Dwarfs , 1971 , pp. 67 - 76
Copyright
Copyright © Reidel 1971 

References

Eggen, O. J. and Greenstein, J. L.: 1965, Astrophys. J. 141, 83.Google Scholar
Eggen, O. J. and Greenstein, J. L.: 1967, Astrophys. J. 150, 927.Google Scholar
Greenstein, J. L.: 1958, Encyclopedia of Physics 50, 161, Springer-Verlag, Berlin.Google Scholar
Greenstein, J. L.: 1960, Stellar Atmospheres (ed. by Greenstein, J. L.), University of Chicago Press, Chicago, Chapter xix.Google Scholar
Greenstein, J. L. and Trimble, V. L.: 1967, Astrophys. J. 149, 283.CrossRefGoogle Scholar
Hamada, T. and Salpeter, E. E.: 1961, Astrophys. J. 134, 683.Google Scholar
Kolesov, A. K.: 1964, Soviet Astron. AJ 8, 185.Google Scholar
Kurucz, R. L.: 1969a, Astrophys. J. 156, 235.Google Scholar
Kurucz, R. L.: 1969b, Theory and Observation of Normal Stellar Atmospheres (ed. by Gingerich, O.) MIT Press, Cambridge, p. 375.Google Scholar
Matsushima, S. and Terashita, Y.: 1969, Astrophys. J. 156, 219.CrossRefGoogle Scholar
Oke, J. B.: 1963, paper presented at the Cleveland meeting of the AAAS.Google Scholar
Oke, J. B.: 1969, Publ. Astron. Soc. Pacific 81, 11.CrossRefGoogle Scholar
Oke, J. B. and Schild, R. E.: 1970, Astrophys. J. 161, in press.CrossRefGoogle Scholar
Popper, D. M.: 1954, Astrophys. J. 120, 316.Google Scholar
Schatzman, E.: 1958, White Dwarfs, North-Holland Publ. Co., Amsterdam.Google Scholar
Shipman, H. L. and Strom, S. E.: 1970, Astrophys. J. 159, 183.Google Scholar
Strom, S. E. and Avrett, E. H.: 1964, Astrophys. J. 140, 1381.Google Scholar
Strom, S. E. and Avrett, E. H.: 1965, Astrophys. J. Suppl. 12, 1.CrossRefGoogle Scholar
Terashita, Y. and Matsushima, S.: 1966, Astrophys. J. Suppl. 13, 461.Google Scholar
Terashita, Y. and Matsushima, S.: 1969, Astrophys. J. 156, 203.Google Scholar
Weidemann, V.: 1963, Z. Astrophys. 57, 87.Google Scholar