The radial-velocity curve of V1010 Ophiuchi - Orbital elements and the rotational disturbance

Abstract

Using observations outside eclipse, we have computed new spectroscopic orbital elements for the single-line, eclipsing binary V1010 Oph. With observations inside eclipse, we have identified in the radial-velocity curve the Rossiter-McLaughlin rotational disturbance. Our analysis of the rotational disturbance for V1010 Oph suggests that the instantaneous orbital period of the star for the mean epoch of the eclipse observations is 0.66142298 d while its rotational velocity is 128 km s b The latter value used in combination with the appropriate spectroscopic and photometric data yields unexpectedly small masses for both component stars in the system.

Radial Velocity Studies of Close Binary Stars. XII.

“…Margoni et al (1981) observations led to a significant orbital eccentricity of 0.23 ± 0.03 which is highly unexpected for such a close binary and indicated a problem in the analysis. Later observations of Worek et al (1988) gave a small eccentricity of e = 0.02 ± 0.02 which is consistent with zero due to the biased character of the eccentricity estimates (it cannot be negative). While the previous velocity semi-amplitudes were consistent, the center of mass velocity was discordant, with V 0 = −15 ± 3 km s −1 determined by Margoni et al (1981) and V 0 = −41 ± 1.5 km s −1 determined by Guinan & Koch (1977).…”

“…Its variability was discovered by Strohmeier et al (1964). The published spectroscopic studies of the system (Guinan & Koch 1977;Margoni et al 1981;Worek et al 1988) found V1010 Oph to be a SB1 system with K 1 ≃ 100 km s −1 . Margoni et al (1981) observations led to a significant orbital eccentricity of 0.23 ± 0.03 which is highly unexpected for such a close binary and indicated a problem in the analysis.…”

The 7.5 Magnitude Limit Sample of Bright Short‐Period Binary Stars. I. How Many Contact Binaries Are There?

“…Photometric studies by Leung (1974) and Leung & Wilson (1977). Three SB1 spectroscopic orbits summarized in Worek et al (1988). An attempt to detect spectral lines of the secondary should be made.…”

The Banana Project. Iii. Spin-Orbit Alignment in the Long-Period Eclipsing Binary Ny Cephei

“…References. -(1) Rossiter (1924); (2) Harmanec (2002); (3) Worek et al (1988) (4) Corcoran et al (1991); (5) Twigg (1979); (6) Bakış et al (2006); (7) Worek (1985); (8) Worek (1996); (9) Lázaro et al (2006); (10) Lázaro et al (2004);(11) McLaughlin (1924); (12) Struve & Elvey (1931); ( 13) Soderhjelm (1980); ( 14) Rucinski (2009); (15) Hube & Couch (1982); ( 16) Holmgren et al (1990);(17) This study; (18) Popper (1982); (19) Albrecht et al (2009); (20) Andersen et al (1987); (21) Albrecht et al (2007) developed, it would seem that the mechanisms they propose should also operate in the case of binary stars, and therefore the theories might be tested by measuring the obliquities of binary stars.…”