P Cygni in a short S Doradus phase. Spectroscopic and photometric evidences

Details P Cygni in a short S Doradus phase. Spectroscopic and photometric evidences P Cygni in a short S Doradus phase. Spectroscopic and photometric evidences

Sep 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...376..898m&link_type=abstract

Astronomy and Astrophysics, v.376, p.898-906 (2001)

Astronomy and Astrophysics

Astrophysics

7

Stars: Oscillations, Stars: Mass Loss, Stars: Individual: P Cygni

Scientific paper

We studied the long-term spectral and photometric behaviour of P Cygni over the 13.8 year interval from March 1985 to January 1999. The UBV photometry reveals a slow ( ~ 7.4-year), low-amplitude ( ~ 0.1 mag) variation in V in which the star becomes redder when it brightens and vice versa. It underwent a possible maximum in the winter of 1985 (between JD 2 446 000 and JD 2 446 200), a minimum in the winter of 1989 (between JD 2 447 500 and JD 2 447 700), a maximum in the fall of 1992 (between JD 2 448 800 and JD 2 449 000), and a minimum in the spring of 1996 (between JD 2 450 100 and JD 2 450 300) The properties of this variation are typical for weak-active S Dor variables in ``short S Dor phase'' \citep{vanGen01}. Simultaneous spectroscopic observations show changes in the Hα equivalent width (corrected for the effect of the changing continuum) in positive correlation with the 7.4-year photometric oscillation in the V-band brightness. This result is interpreted as an indication that in P Cygni an increase in the stellar brightness, during the 7.4-year SD phase, is likely accompanied by an increase in the mass-loss rate. In this behaviour P Cygni is similar to S Dor and R71. From simple considerations, it is concluded that the 7.4-year SD cycle is probably a combination of an increasing radius/decreasing effective temperature and an expanding pseudo-photosphere.

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