Period changes and a possible second pulsation mode in BW Vulpeculae

Details Period changes and a possible second pulsation mode in BW Vulpeculae Period changes and a possible second pulsation mode in BW Vulpeculae

Aug 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984pasp...96..657o&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 96, Aug. 1984, p. 657-660.

Astronomy and Astrophysics

Astronomy

18

Binary Stars, Cepheid Variables, Stellar Oscillations, Astronomical Photometry, Companion Stars

Scientific paper

A new quadratic ephemeris has been derived for the high-amplitude beta-Cephei pulsator BW Vulpeculae based on observations through eight photometric maxima during 1980-1981. An examination of the collected data for the historic maxima shows reveals a cyclic variation of the residuals (O-C) with a period of nearly 25 years and an amplitude of 17 minutes. Two hypotheses are offered to explain the phenomenon: (1) the light travel time accross a binary orbit; or (2) a beating between two pulsation modes with identical periods. It is shown that a secondary companion star with 0.8 to 2.5 solar mass at a distance of 17 to 24 AU would be enough to cause such a fluctuation. Yearly photoelectric observations of BW Vul are recommended in order to determine the period of the variation in the pulsation modes.

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