Hostname: page-component-78c5997874-j824f Total loading time: 0 Render date: 2024-11-20T05:45:16.976Z Has data issue: false hasContentIssue false
  • English
  • Français

Nova Cygni 1975: A Model for the Variability of the 3 Hour Period

Published online by Cambridge University Press:  12 April 2016

A.C. Fabian  and
J. E. Pringle
A.C. Fabian
Affiliation:
Institute of Astronomy, Cambridge, U.K.
J. E. Pringle
Affiliation:
Institute of Astronomy, Cambridge, U.K.

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.

A periodic modulation in the optical flux from Nova Cygni 1975 has been observed since shortly after outburst (Tempesti 1975) and the period is known to have varied by at least a few percent (Semeniuk et al. 1976). We account for the modulation in terms of a simple geometrical model in which the wind emanating from the nova is shadowed by its binary companion (see Fabian and Pringle 1977 for a fuller account). This produces an azimuthal variation in the radius of the surface of last scattering, RS, which an observer sees as a periodic modulation of the. continuum with period roughly equal to the orbital period. Variation of the observed period is accounted for in terms of variation of the size of RS.

Type
Part II: Cataclysmic Variables
Information
International Astronomical Union Colloquium , Volume 42: The Interaction of Variable Stars with their Environment , 1977 , pp. 311 - 312
Copyright
Copyright © Veröff. Der Remeis-Sterwarte 1977

References

Fabian, A.C. and Pringle, J.E., 1977, Mon. Not. R. Astr. Soc. 180, 749.Google Scholar
Semeniuk, I., Kruszewski, A. and Schwarzenberg-Czerny, A., 1976, Inf. Bull. Var. Stars No. 1157.Google Scholar
Tempesti, P. 1975, I.A.U. Circ. No. 2834.Google Scholar