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HD 161306: a radiatively interacting Be binary?
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SYSNO ASEP 0433681 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title HD 161306: a radiatively interacting Be binary? Author(s) Koubský, Pavel (ASU-R) RID, ORCID
Kotková, Lenka (ASU-R)
Kraus, Michaela (ASU-R) RID, ORCID
Yang, S. (CA)
Šlechta, Miroslav (ASU-R) RID, ORCID
Harmanec, P. (CZ)
Wolf, M. (CZ)
Votruba, Viktor (ASU-R) RID
Kubát, Jiří (ASU-R) RID, ORCID
Kubátová, Brankica (ASU-R) RID, ORCID
Niemczura, E. (PL)
Škoda, Petr (ASU-R) RID, ORCIDSource Title Astronomy & Astrophysics. - : EDP Sciences - ISSN 0004-6361
Roč. 567, July (2014), A57/1-A57/4Number of pages 4 s. Publication form Print - P Language eng - English Country FR - France Keywords binaries: spectroscopic ; stars: emission-line ; Be: stars Subject RIV BN - Astronomy, Celestial Mechanics, Astrophysics R&D Projects GA14-21373S GA ČR - Czech Science Foundation (CSF) LG14026 GA MŠMT - Ministry of Education, Youth and Sports (MEYS) Institutional support ASU-R - RVO:67985815 UT WOS 000341185300144 DOI 10.1051/0004-6361/201424022 Annotation The spectrum of the Be star HD 161306 is shown to vary periodically with a period close to 100 days. The radial velocity of the He I 6678 A emission peak varying in antiphase to the radial velocity of the Halpha emission wings component suggests that the star is a binary similar to phi Per, 59 Cyg, or FY CMa, i.e. a radiatively 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, 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. Workplace Astronomical Institute Contact Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Year of Publishing 2015
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