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o Puppis: another Be plus sdO binary?
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DOI：10.1051/0004-6361/201219679.png)
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The spectrum of the Be star o Pup is shown to vary periodically with a period of 28.9 days. A radial-velocity variable He I 6678 angstrom emission component suggests that the star is the same type as phi Per, 59 Cyg, and FY CMa, i.e. binaries consisting of a Be star and a hot companion that illuminates the Be star disk (also called phi Per-type binaries or Be+sdO binaries). The range of radial-velocity variations of the stronger emission component in the helium line observed in o Pup is about 270 km s(-1), a value in good agreement with the range derived for phi Per-type binaries. The radial velocity curves defined by the prominent emission peak in He I 6678 angstrom line and H alpha + Paschen emission move in anti-phase. We suggest that o Pup is generically similar to phi Per-type systems and may represent the fourth case of a Be star with a hot subdwarf companion.
Keyword:
binaries: spectroscopic
stars: emission-line
Be-stars: individual: o Puppis
binaries: close
期刊
IF:
5.8
论文数:
5.0W
被引数:
18.3W
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引用论文
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