Статья

Radial Velocity Studies of Close Binary Stars. XII.

Theodor PribullaAstronomical Institute of the Slovak Academy of SciencesSlavek M. RucinskiDavid Dunlap Observatory, University of Toronto, Richmond Hill, ON L4C 4Y6, CanadaGeorge ConidisDavid Dunlap Observatory, University of Toronto, Richmond Hill, ON L4C 4Y6, CanadaHeide DeBondDavid Dunlap Observatory, University of Toronto, Richmond Hill, ON L4C 4Y6, CanadaJ. R. ThomsonDavid Dunlap Observatory, University of Toronto, Richmond Hill, ON L4C 4Y6, CanadaKosmas GazeasDepartment of Astrophysics, Astronomy, and Mechanics, National and Kapodistrian University of Athens, 15784 Zographou, Athens, GreeceWaldemar OgłozaMt. Suhora Observatory of the Pedagogical University, 30084 Cracow, Poland

2007en

ABI

Аннотация

Radial-velocity measurements and sine-curve fits to the orbital radial velocity variations are presented for ten close binary systems: OO Aql, CC Com, V345 Gem, XY Leo, AM Leo, V1010 Oph, V2612 Oph, XX Sex, W UMa, and XY UMa. Most of these binaries have been observed spectroscopically before, but our data are of higher quality and consistency than in the previous studies. While most of the studied eclipsing pairs are contact binaries, V1010 Oph is probably a detached or semi-detached double-lined binary and XY UMa is a detached, chromospherically active system whose broadening functions clearly show well defined and localized dark spots on the primary component. A particularly interesting case is XY Leo, which is a member of visually unresolved quadruple system composed of a contact binary and a detached, non-eclipsing, active binary with 0.805 days orbital period. V345 Gem and AM Leo are known members of visual binaries. We found faint visual companions at about 2-3 arcsec from XX Sex and XY UMa.

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Идентификаторы

DOI: 10.1086/512772

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