Hostname: page-component-cb9f654ff-mwwwr Total loading time: 0 Render date: 2025-09-07T23:18:13.038Z 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, Arizona 85721
J.B. Holberg
Affiliation:
Lunar and Planetary Laboratory, University of Arizona Tucson, Arizona 85721
F. Wesemael
Affiliation:
Département de Physique and Observatoire du Mont Mégantic Université de 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.

Information

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