Home • Search • Translate
From Wikipedia, the free encyclopedia
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
SIMBAD data

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.
Retrieved from " https://en.wikipedia.org/?title=RV_Corvi&oldid=1206416716"
From Wikipedia, the free encyclopedia
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
SIMBAD data

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.
Retrieved from " https://en.wikipedia.org/?title=RV_Corvi&oldid=1206416716"

Videos

Youtube | Vimeo | Bing

Websites

Google | Yahoo | Bing

Encyclopedia

Google | Yahoo | Bing

Facebook




Top Of Page

Home • Search • Translate

© CSE