SX Corvi

SX Corvi is an eclipsing binary star system in the constellation Corvus, ranging from apparent magnitude 8.99 to 9.25 over 7.6 hours.^[2] The system is a contact binary also known as a W Ursae Majoris variable, where the two component stars orbit closely enough to each other for mass to have been transferred between them—in this case the secondary having transferred a large amount of mass to the primary.^[4]

SX Corvi

SX Corvi in the near-infrared Credit: ESO/VHS
Observation data Epoch J2000.0      Equinox J2000.0
Constellation	Corvus
Right ascension	12h 40m 15.04406s[1]
Declination	−18° 48′ 00.9336″[1]
Apparent magnitude (V)	8.99 - 9.25 [2]
Characteristics
Spectral type	F7V[2]
Variable type	W UMa
Astrometry
Radial velocity (Rv)	8.71 ± 0.94 km/s
Proper motion (μ)	RA: 39.16 ± 1.21 mas/yr Dec.: -6.07 ± 0.80 mas/yr
Parallax (π)	10.94±1.18 mas[3]
Distance	approx. 300 ly (approx. 91 pc)
Details
Age	7.32 ± 0.97[4] Gyr
Other designations
SX Corvi, HD 110139, HIP 61825, SAO 157434
Database references
SIMBAD	data

Yildiz and colleagues estimated the age of the system at 7.32 ± 0.97 billion years based on study of the properties of the system and estimated rate of mass transfer. They found the current masses of the primary and secondary to be 1.25 ± 0.04 and 0.10 ± 0.01 solar masses respectively, from their original masses of 0.72 ± 0.02 and 1.68 ± 0.05 solar masses.^[4]

A lightcurve of SX Corvi, plotted from Hipparcos data