SX Corvi
Eclipsing binary star in the constellation Corvus
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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 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]
