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Eclipsing binary star in the constellation Corvus From Wikipedia, the free encyclopedia
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.[3] 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.[5]
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Corvus |
Right ascension | 12h 40m 15.04406s[2] |
Declination | −18° 48′ 00.9336″[2] |
Apparent magnitude (V) | 8.99 - 9.25 [3] |
Characteristics | |
Spectral type | F7V[3] |
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[4] |
Distance | approx. 300 ly (approx. 91 pc) |
Details | |
Age | 7.32 ± 0.97[5] Gyr |
Other designations | |
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.[5]
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