Alpha Corvi
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Corvus |
| Right ascension | 12h 08m 24.81652s[1] |
| Declination | −24° 43′ 43.9504″[1] |
| Apparent magnitude (V) | 4.03[2] |
| Characteristics | |
| Spectral type | F1 V[3] |
| U−B color index | +0.00[2] |
| B−V color index | +0.34[2] |
| Astrometry | |
| Radial velocity (Rv) | +3.0[4] km/s |
| Proper motion (μ) | RA: 99.52[1] mas/yr Dec.: −39.19[1] mas/yr |
| Parallax (π) | 66.95 ± 0.15[1] mas |
| Distance | 48.7 ± 0.1 ly (14.94 ± 0.03 pc) |
| Absolute magnitude (MV) | 3.25[5] |
| Details | |
| Mass | 1.39[6] M☉ |
| Luminosity | 4.91[7] L☉ |
| Surface gravity (log g) | 4.13 ± 0.05[8] cgs |
| Temperature | 7,041 ± 53[8] K |
| Metallicity [Fe/H] | −0.19 ± 0.04[8] dex |
| Rotational velocity (v sin i) | 16.9 ± 1.5[9] km/s |
| Other designations | |
Alpha Corvi (α Corvi, abbreviated Alpha Crv, α Crv), also named Alchiba,[11] is a star in the constellation of Corvus.
Nomenclature
α Corvi (Latinised to Alpha Corvi) is the star's Bayer designation.
It bore the traditional names Alchiba (Arabic ألخبا al-xibā "tent") and Al Minliar al Ghurab (Arabic منقار الغراب al-manxar al-ghurab) or Minkar al Ghurab. The latter appeared in the catalogue of stars in the Calendarium of Al Achsasi al Mouakket, which was translated into Latin as Rostrum Corvi (beak of the crow).[12] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[13] to catalogue and standardize proper names for stars. The WGSN approved the name Alchiba for this star on 12 September 2016 and it is now so entered in the IAU Catalog of Star Names.[11]
In Chinese astronomy, Alchiba is called 右轄, Pinyin: Yòuxiá, meaning Right Linchpin, because it stands alone in the Right Linchpin asterism, Chariot mansion (see: Chinese constellation),[14] 右轄 (Yòuxiá), westernized into Yew Hea by R.H. Allen.[15]
Namesake
USS Alchiba (AKA-6) is a former United States Navy ship.
Properties
Alchiba belongs to the spectral class F1V and has apparent magnitude +4.00. It is 48.7 ± 0.1 light years from Earth.[1] This star exhibits periodic changes in its spectrum over a three-day period, which suggests it is either a spectroscopic binary or (more likely) a pulsating Gamma Doradus-type variable.[6]
See also
References
- 1 2 3 4 5 6 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752
, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357 - 1 2 3 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data, SIMBAD, Bibcode:1986EgUBV........0M.
- ↑ Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637.
- ↑ Nordström, B.; 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, Bibcode:2004PASA...21..129N, doi:10.1071/AS04013.
- ↑ Elgarøy, Øystein; Engvold, Oddbjørn; Lund, Niels (March 1999), "The Wilson-Bappu effect of the MgII K line - dependence on stellar temperature, activity and metallicity", Astronomy and Astrophysics, 343: 222–228, Bibcode:1999A&A...343..222E.
- 1 2 Fuhrmann, K.; Chini, R. (2012). "Multiplicity among F-type Stars". The Astrophysical Journal Supplement. 203 (2): 20. Bibcode:2012ApJS..203...30F. doi:10.1088/0067-0049/203/2/30. 30.
- ↑ McDonald, I.; Zijlstra, A. A.; Boyer, M. L. (2012). "Fundamental Parameters and Infrared Excesses of Hipparcos Stars". Monthly Notices of the Royal Astronomical Society. 427 (1): 343–57. arXiv:1208.2037. Bibcode:2012MNRAS.427..343M. doi:10.1111/j.1365-2966.2012.21873.x.
- 1 2 3 Prugniel, P.; Vauglin, I.; Koleva, M. (2011). "The atmospheric parameters and spectral interpolator for the MILES stars". Astronomy & Astrophysics. 531: A165. arXiv:1104.4952. Bibcode:2011A&A...531A.165P. doi:10.1051/0004-6361/201116769.
- ↑ Ammler-von Eiff, M.; Reiners, A. (2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: 31, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, A116.
- ↑ "alf Crv -- Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2014-05-20.
- 1 2 "IAU Catalog of Star Names". Retrieved 28 July 2016.
- ↑ Knobel, E. B. (June 1895), "Al Achsasi Al Mouakket, on a catalogue of stars in the Calendarium of Mohammad Al Achsasi Al Mouakket", Monthly Notices of the Royal Astronomical Society, 55: 429, Bibcode:1895MNRAS..55..429K, doi:10.1093/mnras/55.8.429.
- ↑ IAU Working Group on Star Names (WGSN), International Astronomical Union, retrieved 22 May 2016.
- ↑ (Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 22 日
- ↑ Allen, Richard Hinckley, Star Names — Their Lore and Meaning: Corvus.
External links
- Alpha Corvi by Professor Jim Kaler.