VV Corvi

A light curve for VV Corvi, plotted from TESS data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Corvus
Right ascension 12h 41m 15.9528s[2]
Declination −13° 00′ 50.044″[3]
Apparent magnitude (V) 5.27[3]
Characteristics
Spectral type F5IV[3]
U−B color index +0.10[4]
B−V color index +0.42[4]
Astrometry
Radial velocity (Rv)-19.0[5] km/s
Proper motion (μ) RA: -117.92[2] mas/yr
Dec.: 7.86[2] mas/yr
Parallax (π)11.72 ± 1.90 mas[2]
Distanceapprox. 280 ly
(approx. 90 pc)
Other designations
BD−12° 3676, HD 110317, HIP 61910, HR 4821.[3]
Database references
SIMBADdata

VV Corvi (abbreviated as VV Crv) is a close spectroscopic binary in the constellation Corvus. It is also an eclipsing binary, varying from magnitude 5.19 to 5.34 over 3.145 days.[6] The two stars orbit each other with a period of 1.46 days and an eccentricity of 0.088.[7] The mass ratio of the two stars is 0.775±0.024.[8] The primary is 1.978 ± 0.010 times as massive as the Sun, 18.253 ± 2.249 its luminosity and has 3.375 ± 0.010 the Sun's radius. The secondary is 1.513 ± 0.008 times as massive as the Sun, 4.745 ± 0.583 its luminosity and has 1.650 ± 0.008 the Sun's radius. Both are yellow-white main sequence stars of spectral type F5V, though the primary has begun expanding and cooling as it nears the end of its time on the main sequence.[9] A tertiary companion was discovered during the Two Micron All-Sky Survey.[10]

The system shares a common proper motion with HR 4822, which is 5"2 away.[9]

References

  1. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. 1 2 3 4 Perryman, M. A. C.; et al. (1997). "The Hipparcos Catalogue". Astronomy and Astrophysics. 323: L49–L52. Bibcode:1997A&A...323L..49P.
  3. 1 2 3 4 "V* VV Crv -- Spectroscopic binary". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2009-04-19.
  4. 1 2 Johnson, H. L.; Iriarte, B.; Mitchell, R. I.; Wisniewskj, W. Z. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Lab, 4 (3): 99, Bibcode:1966CoLPL...4...99J
  5. ↑ Nordström, B.; Andersen, J.; Holmberg, J.; Jørgensen, B. R.; et al. (2004). "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ~14000 F and G dwarfs". Publications of the Astronomical Society of Australia. 21 (2): 129–133. arXiv:0811.3982. Bibcode:2004PASA...21..129N. doi:10.1071/AS04013. S2CID 123457673.
  6. ↑ Watson, Christopher (4 January 2010). "VV Corvi". The International Variable Star Index. American Association of Variable Star Observers. Retrieved 5 June 2015.
  7. ↑ Batten, A. H. (1967). "Sixth catalogue of the orbital elements of spectroscopic binary systems". Publications of the Dominion Astrophysical Observatory, Victoria. 13: 119–251. Bibcode:1967PDAO...13..119B.
  8. ↑ Lucy, L. B.; Ricco, E. (March 1979). "The significance of binaries with nearly identical components". Astronomical Journal. 84: 401–412. Bibcode:1979AJ.....84..401L. doi:10.1086/112434.
  9. 1 2 Fekel, Francis C.; Henry, Gregory W.; Sowell, James R. (2013). "Absolute Properties of the Eclipsing Binary VV Corvi". The Astronomical Journal. 146 (6): 9. Bibcode:2013AJ....146..146F. doi:10.1088/0004-6256/146/6/146. 146.
  10. ↑ Tokovinin, A.; Thomas, S.; Sterzik, M.; Udry, S. (2008). "Tertiary companions to close spectroscopic binaries". Multiple Stars Across the H-R Diagram, ESO Astrophysics Symposia. Berlin Heidelberg. p. 129. arXiv:astro-ph/0601518. Bibcode:2006yCat..34500681T. doi:10.1051/0004-6361:20054427. ISBN 978-3-540-74744-4.
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