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RV Corvi

In today's world, RV Corvi has become a topic of great relevance and interest to people of all ages and backgrounds. Whether on a personal, professional, social or cultural level, RV Corvi has captured attention and generated important debates and reflections. Its impact has been felt in different areas of daily life, triggering discussions around its implications and consequences. Over the years, RV Corvi has taken different forms and has evolved depending on the circumstances and trends of the moment, remaining a crucial topic for contemporary society. In this article, we will thoroughly explore the importance of RV Corvi and its influence on various aspects of our lives, offering detailed analysis and insights that invite thought and debate.

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RV Corvi

A light curve for RV Corvi, plotted from TESS data[1]
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Corvus
Right ascension 12h 37m 40.711s[2]
Declination −19° 34′ 40.03″[2]
Apparent magnitude (V) 8.77[3] (8.6 - 9.16)[4]
Characteristics
Evolutionary stage Main sequence
Spectral type F0V[5] (F0 + G0)[6]
B−V color index 0.404±0.026[3]
Variable type β Lyr[7]
Astrometry
Radial velocity (Rv)19.0±4.6[8] km/s
Proper motion (μ) RA: −29.326 mas/yr[2]
Dec.: 8.954 mas/yr[2]
Parallax (π)4.7351±0.0812 mas[2]
Distance690 ± 10 ly
(211 ± 4 pc)
Absolute magnitude (MV)2.32[3]
Orbit[9]
Period (P)0.7473 d
Eccentricity (e)0.00
Periastron epoch (T)2445792.3578
Argument of periastron (ω)
(secondary)		0.00°
Semi-amplitude (K1)
(primary)		64 km/s
Semi-amplitude (K2)
(secondary)		235 km/s
Details
Primary
Mass1.64±0.14[9] M☉
Radius2.16 or 2.18 ± 0.08[9] R☉
Luminosity8.4 or 8.5 ± 0.6[9] L☉
Secondary
Mass0.44±0.03[9] M☉
Radius1.19 or 1.20 ±0.04[9] R☉
Luminosity1.2 or 1.5 ± 0.1[9] L☉
Other designations
RV Crv, BD−18° 3431, HD 109796, HIP 61620[10]
Database references
SIMBADdata

RV Corvi is an eclipsing binary star system in the southern constellation of Corvus. The brightness of the pair regularly ranges in apparent visual magnitude from 8.6 down to 9.16 over a period 18 hours,[4] even the brightest of which is too faint to be visible to the naked eye. The system is located at a distance of approximately 690 light-years from the Sun based on parallax measurements, and is drifting further away with a radial velocity of ~19 km/s.[8]

The variability of this system was discovered by H. H. Swope.[11] In 1942, Irene G. Buttery published an orbital period of 0.74728 days for the system, showing this is an eclipsing binary.[12] It is a near-contact binary with both stars showing the effect of tidal interactions and the facing sides are less than 10% of the orbital separation apart, but are not in contact.[13] One or both stars may show an excess of luminosity on their facing sides.[9] The system is composed of stars of spectral types F0 and G0, which orbit each other every 0.7473 days.[6]

References

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  2. ^ a b c d Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  3. ^ a b c Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  4. ^ a b Watson, Christopher (4 January 2010). "RV Corvi". The International Variable Star Index. American Association of Variable Star Observers. Retrieved 21 July 2015.
  5. ^ Houk, Nancy; Smith-Moore, M. (1978). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 4. Ann Arbor: Dept. of Astronomy, University of Michigan. Bibcode:1988mcts.book.....H.
  6. ^ a b Malkov, O. Yu.; et al. (2006). "A catalogue of eclipsing variables". Astronomy and Astrophysics. 446 (2): 785–89. Bibcode:2006A&A...446..785M. doi:10.1051/0004-6361:20053137. hdl:10995/73280.
  7. ^ Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID 125853869. Retrieved 2021-11-27.
  8. ^ a b Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv:1606.08053. Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID 119231169.
  9. ^ a b c d e f g h McFarlane, T. M.; et al. (December 1986). "Contact and near-contact binary systems - V. RV Corvi". Monthly Notices of the Royal Astronomical Society. 223 (3): 595–606. Bibcode:1986MNRAS.223..595M. doi:10.1093/mnras/223.3.595.
  10. ^ "RV Crv". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 21 July 2015.
  11. ^ Abhyankar, K. D.; Parthasarathy, M.; Sanwal, N. B.; Sarma, M. B. K. (January 1974). "UBV photometry of RV CrV". Astronomy and Astrophysics Supplement. 13: 101. Bibcode:1974A&AS...13..101A.
  12. ^ Buttery, Irene G. (1942). "Twenty-two new variable stars in MWF 10". Annals of Harvard College Observatory. 109: 25–26. Bibcode:1942AnHar.109...25B.
  13. ^ Shaw, J. Scott; et al. (April 1996). "Near-Contact Binary Systems in the ROSAT All-Sky Survey". Astrophysical Journal. 461: 951. Bibcode:1996ApJ...461..951S. doi:10.1086/177116.
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