HD 161306: a radiatively interacting Be binary?

Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F14%3A10286177" target="_blank" >RIV/00216208:11320/14:10286177 - isvavai.cz</a>
Alternative codes found
RIV/67985815:_____/14:00433681 RIV/00216224:14310/14:00107094
Result on the web
<a href="http://dx.doi.org/10.1051/0004-6361/201424022" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201424022</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1051/0004-6361/201424022" target="_blank" >10.1051/0004-6361/201424022</a>

Result language
angličtina
Original language name
HD 161306: a radiatively interacting Be binary?
Original language description
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.
Czech name
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Czech description
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Type
J<sub>x</sub> - Unclassified - Peer-reviewed scientific article (Jimp, Jsc and Jost)
CEP classification
BN - Astronomy and celestial mechanics, astrophysics
OECD FORD branch
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Project
Result was created during the realization of more than one project. More information in the Projects tab.
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Publication year
2014
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

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