SX Corvi

SX Corvi is an eclipsing binary star system in the constellation Corvus, ranging from apparent magnitude 8.99 to 9.25 over 7.5 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
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[3] mas
Distanceapprox. 300 ly
(approx. 91 pc)
Details
Age7.32 ± 0.97[4] Gyr
Other designations
SX Corvi, HD 110139, HIP 61825, SAO 157434
Database references
SIMBADdata

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]

References
  1. "SX Crv -- Eclipsing binary of W UMa type (contact binary)". Retrieved 21 July 2015.
  2. Watson, Christopher (19 April 2012). "SX Corvi". The International Variable Star Index. American Association of Variable Star Observers. Retrieved 21 July 2015.
  3. van Leeuwen, F. (2007). "Validation of the New Hipparcos Reduction". Astronomy and Astrophysics. 474 (2): 653–64. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357.
  4. Yildiz (2014). "Origin of W UMa-type contact binaries - age and orbital evolution". Monthly Notices of the Royal Astronomical Society. 437 (1): 185–94. arXiv:1310.5526. Bibcode:2014MNRAS.437..185Y. doi:10.1093/mnras/stt1874.


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