| 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] |
| Distance | 690 ± 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 | |
| Mass | 1.64±0.14 [9] M☉ |
| Radius | 2.16 or 2.18 ± 0.08 [9] R☉ |
| Luminosity | 8.4 or 8.5 ± 0.6 [9] L☉ |
| Secondary | |
| Mass | 0.44±0.03 [9] M☉ |
| Radius | 1.19 or 1.20 ±0.04 [9] R☉ |
| Luminosity | 1.2 or 1.5 ± 0.1 [9] L☉ |
| Other designations | |
| 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
- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ 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.
- ^ 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.
- ^ a b Watson, Christopher (4 January 2010). "RV Corvi". The International Variable Star Index. American Association of Variable Star Observers. Retrieved 21 July 2015.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ "RV Crv". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 21 July 2015.
- ^ 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.
- ^ Buttery, Irene G. (1942). "Twenty-two new variable stars in MWF 10". Annals of Harvard College Observatory. 109: 25–26. Bibcode: 1942AnHar.109...25B.
- ^ 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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| 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] |
| Distance | 690 ± 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 | |
| Mass | 1.64±0.14 [9] M☉ |
| Radius | 2.16 or 2.18 ± 0.08 [9] R☉ |
| Luminosity | 8.4 or 8.5 ± 0.6 [9] L☉ |
| Secondary | |
| Mass | 0.44±0.03 [9] M☉ |
| Radius | 1.19 or 1.20 ±0.04 [9] R☉ |
| Luminosity | 1.2 or 1.5 ± 0.1 [9] L☉ |
| Other designations | |
| 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
- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ 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.
- ^ 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.
- ^ a b Watson, Christopher (4 January 2010). "RV Corvi". The International Variable Star Index. American Association of Variable Star Observers. Retrieved 21 July 2015.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ "RV Crv". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 21 July 2015.
- ^ 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.
- ^ Buttery, Irene G. (1942). "Twenty-two new variable stars in MWF 10". Annals of Harvard College Observatory. 109: 25–26. Bibcode: 1942AnHar.109...25B.
- ^ 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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| Galaxies |
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