Journal
ASTRONOMY & ASTROPHYSICS
Volume 567, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201424022
Keywords
binaries: spectroscopic; stars: emission-line, Be; stars: individual: HD 161306
Categories
Funding
- ESA [PECS 98058]
- MSMT CR [LG14032]
- GA CR [14-21373S, P209/10/0715]
- NCN [2011/01/B/ST9/05448]
- [1007/S/IAs/14]
- [RVO:67985815]
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The spectrum of the Be star HD 161306 is shossai to Vary periodically with a period of similar to 100 days. The radial velocity of the Het 6678 A emission peak varying in antiphase to the radial velocity of the Ha emission wings component suggests that the star is a binary similar to phi Per, 59 Cyg, or FY CMa, i.e. a radiativelv interacting Be binary - a rare case among Be stars. This type of object is also called a phi Per-type binary or Be + sdO binaries. The range of radial-velocity variations of the strong emission peak in the helium line observed in HD 161306 is about 180 km s(-1), similar to what is observed for these systems. We therefore conclude that HD 161306 may represent another case of a Be star with a hot subdwarf companion.
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