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The absence of a short period in the WN5 star EZ Canis Majoris

Published online by Cambridge University Press:  07 August 2017

Igor I. Antokhin
Affiliation:
Sternberg State Astronomical Institute, Universitetskij pr., 13, Moscow, 119899, Russia
Jean-François Bertrand
Affiliation:
Sternberg State Astronomical Institute, Universitetskij pr., 13, Moscow, 119899, Russia
Robert Lamontagne
Affiliation:
Sternberg State Astronomical Institute, Universitetskij pr., 13, Moscow, 119899, Russia
Anthony F.J. Moffat
Affiliation:
Département de Physique, Université de Montreal, C.P. 6128, Succ. Centre- Ville, Montréal, QC H3C 3J7, and Observatoire du Mont Mégantic, Canada

Extract

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Several suggestion have been put forward to explain the 3.d766 periodicity of EZ CMa (WR6): (i) WR+c system; (ii) rotating single WR star; (iii) pulsations (non—radial (NRP) or radial) with frequency reduced by some kind of filtering in the wind. In this paper, we report on a photometric investigation based on a long continuous observing run, in an attempt to verify whether EZ CMa does in fact show a unique periodicity. In particular, this work was motivated by the claim by Gosset & Vreux (1987), based on the data from Lamontagne et al. (1986, hereafter LML), that EZ CMa may have a shorter period besides the one at 3.d766, a frequency close to but not equal to the third harmonic of the 3.d766 period.

Type
Session I - Basic parameters, properties of single Wolf-Ray et stars
Copyright
Copyright © Kluwer 1995 

References

Antokhin, I.I., Bertrand, J.-F., Lamontagne, R., Moffat, A.F.J. 1994, A J 107, 2179 CrossRefGoogle Scholar
Gosset, E., Vreux, J.M. 1987, A&A 178, 153 Google Scholar
Lamontagne, R., Moffat, A.F.J., Lamarre, A. 1986, AJ 91, 925 (LML) Google Scholar