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

  • Igor I. Antokhin (a1), Jean-François Bertrand (a1), Robert Lamontagne (a1) and Anthony F.J. Moffat (a2)

Extract

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.

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References

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

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

  • Igor I. Antokhin (a1), Jean-François Bertrand (a1), Robert Lamontagne (a1) and Anthony F.J. Moffat (a2)

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