Hostname: page-component-76fb5796d-45l2p Total loading time: 0 Render date: 2024-04-25T14:34:40.500Z Has data issue: false hasContentIssue false
  • English
  • Français

KQ Mon and the Nature of the UX Ursa Majoris Nova-Like Variables

Published online by Cambridge University Press:  12 April 2016

Edward M. Sion  and
Edward F. Guinan
Edward M. Sion
Affiliation:
Astronomy Department, Villanova University
Edward F. Guinan
Affiliation:
Astronomy Department, Villanova University

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.

KQ Mon, a new UX UMa type nova-like variable discovered by H.E. Bond, exhibits optical spectra, UBV and high speed photometric characteristics strongly similar to other members of the UX Ursa Majoris subset. However its ultraviolet spectra when compared with other UX UMa stars shed considerable light on the nature of these objects. Its spectrum is dominated by strong broad highly ionized absorption lines including the NV, SiIV and CIV UV resonance doublets. No emission lines or P Cygni type features are evident and the velocity displacements are smaller suggesting the absence of a hot high velocity wind characterizing other UX UMa stars. A physical interpretation of the UV absorption spectra and optical spectra and their observed temporal variations is presented. Based upon (1) high mass accretion rates derived by fitting the observations with theoretical continuum fluxes from steady accretion disk models by R.E. Williams, (2) the presence of outflowing winds with the determination of corresponding mass loss rates and properties of the theoretical wind models by Cassinelli, Olson and Stalio, and (3) new time independent steady state disk structure computations, a model is suggested to explain the observed properties of the UX UMa stars and their lack of major outbursts.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 72: Cataclysmic Variables and Related Objects , 1983 , pp. 41 - 49
Copyright
Copyright © Reidel 1983

References

REFERENCES

Bath, G.T., and Pringle, J.E.: 1981, Monthly Notices Roy. Astron. Soc. 194, p. 967.Google Scholar
Bond, H.E.: 1978, Publ. Astron. Soc. Pacific 90, p. 216.Google Scholar
Bond, H.E.: 1981 (private communication).Google Scholar
Bond, H.E.: 1982 (unpublished observations).Google Scholar
Boggess, A., et al.: 1978, Nature 275, p. 372.Google Scholar
Cassinelli, J.P., Olson, G.L., and Stallo, R.: 1978, Astrophys. J. 220, p. 573.Google Scholar
Cordova, F.A., Mason, K.O., and Nelson, J.E.: 1981, Astrophys. J. 245, p. 609.Google Scholar
Greenstein, J.B., and Oke, J.B.: 1982, Astrophys. J. 258, p. 209.CrossRefGoogle Scholar
Guinan, E.F., and Sion, E.M.: 1982a, Astrophys. J. 258, p. 217.Google Scholar
Guinan, E.F., and Sion, E.M.: 1982b, “Advances in Ultraviolet Astronomy: Four Years of IUE Research,” NASA Conf. Publ. 2238, p. 465.Google Scholar
Hayes, D.S.: 1979, “Dudley Obs. Report” No. 14, p. 297.Google Scholar
Holm, A.V., Panek, R.J., and Schiffer, F.H.: 1982, Astrophys. J. 252, p. L35.Google Scholar
Meyer, F., and Meyer-Hofmeister, E.: 1981, Astron. Astrophys. 104, p. L10.Google Scholar
Nandy, K., Thompson, G.I., Jamar, C., Monfils, A., and Wilson, R.: 1975, Astron. Astrophys. 44, p. 195.Google Scholar
Sion, E.M., and Guinan, E.F.: 1982, “Advances in Ultraviolet Astronomy: Four Years of IUE Research,” NASA Conf. Publ. 2238, p. 460.Google Scholar
Wargau, W., Drechael, H., Rahe, J., and Vogt, N.: 1982, Astron. Astrophys. 110, p. 281.Google Scholar
Warner, B.: 1976, Observatory 96, p. 49.Google Scholar
Warner, B.: 1982 (preprint).Google Scholar
Williams, R.E.: 1981a, Astrophys. J. 235, p. 939.Google Scholar
Williams, R.E.: 1981b (unpublished models). Google Scholar
Vila, S.C.: 1982 (unpublished models).Google Scholar
Williams, P.: 1982 (private communication).Google Scholar