Hostname: page-component-848d4c4894-pjpqr Total loading time: 0 Render date: 2024-06-13T17:38:00.987Z Has data issue: false hasContentIssue false
  • English
  • Français

A New Temperature Determination for Sirius B from IUE: Implications for the Observed Soft X-Ray Fluxes

Published online by Cambridge University Press:  12 April 2016

K. Kidder ,
J.B. Holberg  and
F. Wesemael
K. Kidder
Affiliation:
Lunar and Planetary Laboratory, University of Arizona Tucson, Arizona85721
J.B. Holberg
Affiliation:
Lunar and Planetary Laboratory, University of Arizona Tucson, Arizona85721
F. Wesemael
Affiliation:
Département de Physique and Observatoire du Mont MéganticUniversitéde Montréal

Abstract

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.

We have used IUE archive observations to obtain a new and independent estimate of the effective temperature of Sirius B. In this effort we have modeled the observed Lyman alpha profile of Sirius B as a function of effective temperature and find; Teff = 24,500 ± 500 K. This temperature is in good agreement with a recent result obtained from analysis of EXOSAT soft X-ray spectra of Sirius B. In addition to providing confirmation of the soft X-ray result, this temperature implies that Sirius B is significantly cooler and larger in radius than most previous estimates. The radius, R = 0.090 ± 0.005 R⊙, implied by the lower temperature is well in excess of the radius of fully degenerate star having the mass of Sirius B. This investigation employed a unique set of SWP archive spectra, acquired with Sirius B in the small aperture, which have proved to be free of scattered light contamination from Sirius A.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 114: White Dwarfs , 1989 , pp. 350 - 353
Copyright
Copyright © Springer-Verlag 1989

References

Böhm-tense, E., Dettmann, T., and Kaprandis, S.: 1979, Astrophys. J. (Letters), 232, L189.Google Scholar
Gatewood, G.D., and Gatewood, C.V: 1978, Astrophys. J., 225, 191.Google Scholar
Hamada, T., and Saltpeter, E.E. : 1961, Astrophys. J., 134, 683.Google Scholar
Holberg, J.B., Wesemael, F., and Hubeny, I.: 1984, Astrophys. J., 280, 679.CrossRefGoogle Scholar
Holberg, J.B., Wesemael, F., and Basile, J.: 1986, Astrophys. J., 306, 329.Google Scholar
Mewe, R., Heise, J., Groneschild, E.H.B.M., Brinkman, A.C., Schrijver, J. and Den Boggende, A.J.F.: 1975, Nature Phys. Sci., 256, 711.Google Scholar
Paerels, F.B.S., et al.: 1988, Astrophys. J., 329, 849.Google Scholar
Shipman, H.L. : 1976, Astrophys. J. (Letters), 206, L67.Google Scholar
Thejll, P., and Shipman, H.L. : 1987, Pub. Astron. Soc. Pacific, 98, 922.Google Scholar