The eccentric orbit of the short-period eclipsing binary V 1010 Oph

Margoni, R.; Stagni, R.; Mammano, A.; Illés-Almár, E.

doi:10.1007/bf00655913

Cited by 11 publications

(18 citation statements)

References 3 publications

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“…It was discovered to be a variable star by Margoni & Stagni (1984, their variable #3) Munari et al (1992) gave K = 8.02, J −K = +1.50, almost identical to Allen (1974), suggesting that the cool giant in Hen 2-468 is not intrinsically variable. Henden & Munari (2000) observed Hen 2-468 in quiescence at B = 16.6 and B − V = +1.8 in 1999, in agreement with the Margoni & Stagni (1984) values.…”

Section: Hen 2-468supporting

confidence: 86%

Symbiotic stars on Asiago archive plates. II

Munari

Jurdana-Šepić

2002

A&A

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Abstract. The Asiago photographic archive has been searched for plates containing the symbiotic stars Hen 2-468, QW Sge, LT Del, V407 Cyg, K 3-9, V335 Vul, FG Ser and Draco C-1. A total of 635 plates imaging the program stars have been found and the brightness estimated using the Henden & Munari (2000) UBV(RI)C photometric sequences. These historical data have allowed for the first time the determination of the orbital periods of Hen 2-468 (774 days) and QW Sge (390.5 days), a significant improvement in the orbital period of LT Del (465.6 days) and for V407 Cyg an evaluation of the Mira's pulsation period and complex lightcurve shape in the red (R and I bands). Some previously unknown outbursts have been discovered too.

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Section: Hen 2-468supporting

confidence: 86%

Symbiotic stars on Asiago archive plates. II

Munari

Jurdana-Šepić

2002

A&A

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“…The lines in the KS Per spectrum are not very broad (our estimates give V × sin i ≈ 30 km/s), but the hydrogen deficiency increases the continuum transparency and, thus, creates a crowded absorption "forest", especially in the UV (Kipper and Klochkova 2008). The mean value of the heliocentric radial velocity measured using our spectrum is 6.2 ± 0.4 km/s that is close to the values of the γ -velocity from Heard (1962) and Margoni et al (1988) which are 7 ± 1 km/s and 3 ± 2 km/s respectively.…”

Section: Ks Persupporting

confidence: 65%

An atlas of ground UV spectra of selected stars

Клочкова

Ченцов

Kipper

et al. 2011

Astrophys Space Sci

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We present a spectral atlas of 4 B and A stars containing spectra in a poorly studied spectral range of 305-452 nm. The atlas is based on high resolution (R = 60 000) spectra obtained with the 6 meter telescope (SAO, Russia) combined with the NES-spectrograph. The procedure of spectral lines identification and compilation of the atlas is discussed in detail. Using the spectral data we thoroughly investigated the velocity field in expanding atmospheres and envelopes of hot evolved stars β Ori, α Cyg and supergiant KS Per with the extreme hydrogen deficiency. The complete atlas and list of the identified spectral lines will be available via the astronomical database SIMBAD.

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“…Later observations of Worek et al (1988) gave a small eccentricity of e ¼ 0:02 AE 0:02, which is consistent with zero due to the biased character of the eccentricity estimates (it cannot be negative). While previous velocity semiamplitudes were consistent, the center-of-mass velocities were discordant, with V 0 ¼ À15 AE 3 km s À1 determined by Margoni et al (1981) and V 0 ¼ À41 AE 1:5 km s À1 determined by Guinan & Koch (1977). The photometric analysis of Leung & Wilson (1977) based on the assumption of the Roche model, showed that (1) the primary eclipse is a transit, (2) the eclipses are total, and (3) the system is in marginal contact.…”

Section: V1010 Ophmentioning

confidence: 97%

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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The eccentric orbit of the short-period eclipsing binary V 1010 Oph

Cited by 11 publications

References 3 publications

Symbiotic stars on Asiago archive plates. II

Symbiotic stars on Asiago archive plates. II

An atlas of ground UV spectra of selected stars

Radial Velocity Studies of Close Binary Stars. XII.

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