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3 Corvi

From Wikipedia, the free encyclopedia

3 Corvi
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Corvus
Right ascension 12h 11m 03.83987s[1]
Declination −23° 36′ 08.7221″[1]
Apparent magnitude (V) 5.45[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type A1 V[4]
B−V color index 0.055±0.004[2]
Astrometry
Radial velocity (Rv)+14.41±1.09[5] km/s
Proper motion (μ) RA: −66.853[1] mas/yr
Dec.: −19.826[1] mas/yr
Parallax (π)17.0039 ± 0.1918 mas[1]
Distance192 ± 2 ly
(58.8 ± 0.7 pc)
Absolute magnitude (MV)1.61[2]
Details[5]
Mass2.14[6] M☉
Radius1.87[7] R☉
Luminosity9.55+1.17
−1.04 L☉
Surface gravity (log g)4.12±0.22 cgs
Temperature9,671±329[6] K
Metallicity [Fe/H]+0.17±0.41 dex
Rotational velocity (v sin i)130 km/s
Age907.37+92.96
−899.21 Myr
Other designations
3 Crv, BD22°3305, HD 105850, HIP 59394, HR 4635, SAO 180546[8]
Database references
SIMBADdata

3 Corvi is a single[9] star in the southern constellation of Corvus, located 192 light years away from the Sun.[1] It is visible to the naked eye as a faint, white-hued star with an apparent visual magnitude of 5.45.[2] This object is moving further from the Earth with a heliocentric radial velocity of +14 km/s.[5]

This is an A-type main-sequence star[3] with a stellar classification of A1 V.[4] It has 2.14[6] times the mass of the Sun and 1.87[7] times the Sun's radius. The star is around 900 million years old with a high rate of rotation, showing a projected rotational velocity of 130 km/s.[5] It is radiating ten[5] times the luminosity of the Sun from its photosphere at an effective temperature of 9,671 K.[6] An infrared excess has been detected, suggesting that a debris disk with a temperature of 150 K is orbiting 14.7 AU from the host star.[7]

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Transcription

References

  1. ^ a b c d e f 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.
  2. ^ a b c d 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.
  3. ^ a b Zorec, J.; Royer, F. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  4. ^ a b 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.
  5. ^ a b c d e Iglesias, D.; et al. (October 2018), "Debris discs with multiple absorption features in metallic lines: circumstellar or interstellar origin?", Monthly Notices of the Royal Astronomical Society, 480 (1): 488–520, arXiv:1806.10687, Bibcode:2018MNRAS.480..488I, doi:10.1093/mnras/sty1724, S2CID 119221436.
  6. ^ a b c d David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  7. ^ a b c Cotten, Tara H.; Song, Inseok (July 2016), "A Comprehensive Census of Nearby Infrared Excess Stars", The Astrophysical Journal Supplement Series, 225 (1): 24, arXiv:1606.01134, Bibcode:2016ApJS..225...15C, doi:10.3847/0067-0049/225/1/15, S2CID 118438871, 15.
  8. ^ "3 Crv". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-04-11.
  9. ^ De Rosa, R. J.; et al. (2014), "The VAST Survey - III. The multiplicity of A-type stars within 75 pc", Monthly Notices of the Royal Astronomical Society, 437 (2): 1216, arXiv:1311.7141, Bibcode:2014MNRAS.437.1216D, doi:10.1093/mnras/stt1932, S2CID 88503488.
This page was last edited on 28 November 2023, at 21:58
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