W Corvi is an eclipsing binary star system in the constellation Corvus, ranging from apparent magnitude 11.16 to 12.5 over 9 hours.[3] Its period has increased by 1/4 second over a century. It is an unusual system in that its two stars are very close to each other yet have different surface temperatures and hence thermal transfer is not taking place as expected.[4]

W Corvi

A visual band light curve for W Corvi, adapted from Odell and Cushing (2004)[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Corvus
Right ascension 12h 07m 34.360s[2]
Declination −13° 08′ 59.02″[2]
Apparent magnitude (V) 11.16 - 12.5[3]
Characteristics
Evolutionary stage Beta Lyrae variable
Spectral type G-
Astrometry
Proper motion (μ) RA: -18.8 ± 2.1 mas/yr
Dec.: 18.2 ± 2.1 mas/yr
Details
Other designations
W Corvi, BD−12° 3565
Database references
SIMBADdata

References

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  1. ^ Odell, A. P.; Cushing, G. E. (March 2004). "Changes in the Period and Light Curve of W Corvi". Information Bulletin on Variable Stars. 5514: 1. Bibcode:2004IBVS.5514....1O. Retrieved 17 December 2021.
  2. ^ a b "W Crv -- Eclipsing binary of beta Lyr type (semi-detached)". Retrieved 21 July 2015.
  3. ^ a b Watson, Christopher (4 January 2010). "W Corvi". The International Variable Star Index. American Association of Variable Star Observers. Retrieved 21 July 2015.
  4. ^ Odell, Andrew P. (1996). "Changes in the Period and Light Curve of W Corvi". Monthly Notices of the Royal Astronomical Society. 282 (2): 373–83. Bibcode:1996MNRAS.282..373O. doi:10.1093/mnras/282.2.373.