The Beta Cephei Type Variable Star BW Vulpeculae

Details The Beta Cephei Type Variable Star BW Vulpeculae The Beta Cephei Type Variable Star BW Vulpeculae

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aipc.1043..416f&link_type=abstract

EXPLORING THE SOLAR SYSTEM AND THE UNIVERSE. AIP Conference Proceedings, Volume 1043, pp. 416-417 (2008).

Computer Science

Databases

Astronomical Catalogs, Atlases, Sky Surveys, Databases, Retrieval Systems, Archives, Etc., Astronomical And Space-Research Instrumentation, Ephemerides, Almanacs, And Calendars, Pulsars, Stellar Characteristics And Properties

Scientific paper

The period variation of BW Vulpeculae can be described by the superposition of two separate physical effects: the evolution of the pulsating star characterized by the quadratic ephemeris and the orbital motion in a binary system. The quadratic term describes a secular period change of 2.37s cen-1 and the orbital motion period is 34.67 years. The overall period variation is obtained combining the two effects.

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