A radial velocity study of XY Leonis

Hrivnak, Bruce J.; Milone, Eugene F.; Hill, G. M.; Fisher, W. A.

doi:10.1086/162545

Cited by 16 publications

(10 citation statements)

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“…It is interesting to note that Hrivnak et al (1984) obtained an even smaller K 1 than Barden (1987), only 108 AE 2 km s À1 . This systematic effect is probably due to the previous use of the cross-correlation technique and thus inadequate resolution, leading to a stronger influence of the third component, which is always close to the center-of-mass velocity of the close binary.…”

Section: Xy Leomentioning

confidence: 93%

Radial Velocity Studies of Close Binary Stars. XII.

Pribulla

Ruciński

Conidis

et al. 2007

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Radial velocity measurements and sine-curve fits to the orbital radial velocity variations are presented for 10 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 semidetached 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, noneclipsing, active binary with an 0.805 day orbital period. V345 Gem and AM Leo are known members of visual binaries. We found faint visual companions at about 2 00 Y3 00 from XX Sex and XY UMa.

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Section: Xy Leomentioning

confidence: 93%

Radial Velocity Studies of Close Binary Stars. XII.

Pribulla

Ruciński

Conidis

et al. 2007

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“…These lines were double at quadratures and narrower with respect to the absorption lines. The reliable radial velocity measurements of this partially eclipsing contact and double-lined spectroscopic binary was obtained by Hrivnak et al (1984). After corrections for tidal and eclipse effects they derived the masses of the components as 0.87 and 0.44 solar masses.…”

Section: Introductionmentioning

confidence: 99%

New light curve analysis and period changes of the overcontact binary XY Leonis

Yakut

İbanoǧlu

Kalomeni

et al. 2003

A&A

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Abstract. Light curves and photometric solutions of the contact binary XY Leo are presented. The UBVR light curves appear to be almost symmetric. The B and V light curves were analysed with the Wilson-Devinney code and the orbital parameters of the system were obtained and compared with those obtained in previous studies. All the times of minimum light were collected and combined with the new ones obtained in this study. The orbital period of the system oscillates with a period of 19.6 years and a semi-amplitude of 0.023 day. This regular change was analysed under the assumption of the third body hypothesis. The time delay and advance due to the orbit of the eclipsing pair around the third component were computed and subtracted from the original residuals obtained with the linear light elements. The remaining residuals also show a parabolic change. Therefore, we assumed that the orbital period of the system changes with time due to at least two different causes. The parabolic change of the period may be attributed to either mass transfer from less massive component to the more massive one, or an additional component bounded to the double binary system with a longer period.

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“…In stark contrast to the multitude of photometric studies (Yakut et al 2003, and references therein), only two spectroscopic studies aimed at measuring radial velocity curves (Hrivnak et al 1984;Barden 1987). XY Leo has four components.…”

Section: Xy Leonismentioning

confidence: 99%

Physical parameters and multiplicity of five southern close eclipsing binaries

Szalai

Kiss

Mészáros

et al. 2007

A&A

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Aims. We detected tertiary components of close binaries from spectroscopy and light curve modelling, investigated the lighttravel time effect and the possibility of magnetic activity cycles, measured mass ratios for unstudied systems, and derived absolute parameters. Methods. We carried out new photometric and spectroscopic observations of five bright ( V < 10.5 mag) close eclipsing binaries, predominantly in the southern skies. We obtained full Johnson BV light curves, which were modelled with the Wilson-Devinney code. Radial velocities were measured with the cross-correlation method using IAU radial velocity standards as spectral templates. Period changes were studied with the O−C method, utilising published epochs of minimum light (XY Leo) and ASAS photometry (VZ Lib). Results. For three objects (DX Tuc, QY Hya, V870 Ara), absolute parameters have been determined for the first time. We spectroscopically detected the tertiary components in XY Leo and VZ Lib and discovered one in QY Hya. For XY Leo we updated the light-time effect parameters and detected a secondary periodicity of about 5100 d in the O−C diagram that may hint at the existence of short-period magnetic cycles. A combination of recent photometric data shows that the orbital period of the tertiary star in VZ Lib is likely to be over 1500 d. QY Hya is a semi-detached X-ray active binary in a triple system with K and M-type components, while V870 Ara is a contact binary with the third smallest spectroscopic mass ratio for a W UMa star to date (q = 0.082 ± 0.030). Being close to the theoretical minimum for contact binaries, this small mass ratio suggests that V870 Ara has the potential of constraining evolutionary scenarios of binary mergers. The inferred distances to these systems are compatible with the Hipparcos parallaxes.

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A radial velocity study of XY Leonis

Cited by 16 publications

References 0 publications

Radial Velocity Studies of Close Binary Stars. XII.

Radial Velocity Studies of Close Binary Stars. XII.

New light curve analysis and period changes of the overcontact binary XY Leonis

Physical parameters and multiplicity of five southern close eclipsing binaries

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