Mode Identification of the β Cephei star BW Vulpeculae
نویسندگان
چکیده
منابع مشابه
The close Be star companion of β Cephei
Context. The prototype of the β Cephei class of pulsating stars, β Cep, rotates relatively slowly, and yet displays episodic Hα emission. Such behaviour is typical of a rapidly rotating, classical Be star. For some time this posed a contradiction to our understanding of the Be phenomena as rapid rotation is thought to be a prerequisite for the characteristic emission phases of Be stars. Recent ...
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β Cen is a bright β Cephei variable and has long been suspected to be a binary. Here we report interferometric observations with the 3.9-m Anglo-Australian Telescope at a single epoch which show the star to be a binary with components separated by 15 milliarcsec and having approximately equal luminosities at 486 nm. We also present high-resolution spectra taken over five nights with the ESO CAT...
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Based on new observations, it is shown here that the amplitude of one of the three well known and stable short periods in the β Cep variable 16 Lac has changed: while the radial modeP1 = 0.16917 d is near its lower amplitude level and the amplitude variation of the non-radial mode P3 = 0.18173 d is still probably in phase with the orbital period, the amplitude of the NR mode P2 = 0.17077 d has ...
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ژورنال
عنوان ژورنال: International Astronomical Union Colloquium
سال: 1995
ISSN: 0252-9211
DOI: 10.1017/s0252921100036770