Astronomy:Zeta Centauri
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 13h 55m 32.38565s[1] |
| Declination | −47° 17′ 18.1482″[1] |
| Apparent magnitude (V) | +2.55[2] |
| Characteristics | |
| Spectral type | B2.5 IV[3] |
| U−B color index | −0.91[2] |
| B−V color index | −0.22[2] |
| Astrometry | |
| Radial velocity (Rv) | +6.5[4] km/s |
| Proper motion (μ) | RA: −57.37[1] mas/yr Dec.: −44.55[1] mas/yr |
| Parallax (π) | 8.54 ± 0.13[1] mas |
| Distance | 382 ± 6 ly (117 ± 2 pc) |
| Absolute magnitude (MV) | −2.79[5] |
| Orbit[6] | |
| Period (P) | 8.024 days |
| Semi-major axis (a) | 0.0014"[7] |
| Eccentricity (e) | 0.5 |
| Periastron epoch (T) | 2413719.321 JD |
| Argument of periastron (ω) (secondary) | 290° |
| Details | |
| Mass | 7.8±0.1[3] M☉ |
| Radius | 5.80±0.53[8] R☉ |
| Surface gravity (log g) | 3.84±0.08[8] cgs |
| Temperature | 23561±283[8] K |
| Rotational velocity (v sin i) | 235[9] km/s |
| Age | 39.8±5.7[3] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Zeta Centauri, Latinized from ζ Centauri, is a binary star system in the southern constellation of Centaurus. It has the proper name Alnair /æˈnɛər/, from Arabic: نير بطن قنطورس.[11][12] With a combined apparent visual magnitude of +2.55,[2] it is one of the brighter members of the constellation. This system is close enough to the Earth that its distance can be measured directly using the parallax technique. This yields a value of roughly 382 light-years (117 parsecs), with a 1.6% margin of error.[1] It is drifting further away with a radial velocity of +6.5 km/s.[4]
In Chinese, 庫樓 (Kù Lóu), meaning Arsenal, refers to an asterism consisting of ζ Centauri, η Centauri, θ Centauri, 2 Centauri, HD 117440, ξ1 Centauri, γ Centauri, τ Centauri, D Centauri and σ Centauri.[13] Consequently, the Chinese name for ζ Centauri itself is 庫樓一 (Kù Lóu yī, English: the First Star of Arsenal.)[14]
ζ Cen is a double-lined spectroscopic binary system,[15] which indicates that the orbital motion was detected by shifts in the absorption lines of their combined spectra caused by the Doppler effect. The two stars orbit each other over a period of slightly more than eight days with an orbital eccentricity of about 0.5.[6] The estimated angular separation of the pair is 1.4 mas.[7]
At an estimated age of 40 million years,[3] the primary component of this system appears to be in the subgiant stage of its evolution with a stellar classification of B2.5 IV.[3] It is a large star with nearly 8[3] times the mass of the Sun and close to 6[8] times the Sun's radius. This star is rotating rapidly with a projected rotational velocity of 235 km s−1.[9]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V
- ↑ 2.0 2.1 2.2 2.3 Johnson, H. L. et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory 4 (99): 99, Bibcode: 1966CoLPL...4...99J
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society 410 (1): 190–200, doi:10.1111/j.1365-2966.2010.17434.x, Bibcode: 2011MNRAS.410..190T
- ↑ 4.0 4.1 Wilson, R. E. (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication (Carnegie Institute of Washington D.C.), Bibcode: 1953GCRV..C......0W
- ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 6.0 6.1 Maury, A. C. (1922), "The Orbit of the Spectroscopic Binary ζ Centauri", Harvard College Observatory Circular 233: 1–4, Bibcode: 1922HarCi.233....1M
- ↑ 7.0 7.1 Halbwachs, J. L. (April 1981), "List of Estimated Angular Separations of Spectroscopic Binaries", Astronomy and Astrophysics Supplement 44: 47, Bibcode: 1981A&AS...44...47H
- ↑ 8.0 8.1 8.2 8.3 Fitzpatrick, E. L.; Massa, D. (March 2005), "Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry", The Astronomical Journal 129 (3): 1642–1662, doi:10.1086/427855, Bibcode: 2005AJ....129.1642F
- ↑ 9.0 9.1 Bernacca, P. L.; Perinotto, M. (1970), "A catalogue of stellar rotational velocities", Contributi Osservatorio Astronomico di Padova in Asiago 239 (1): 1, Bibcode: 1970CoAsi.239....1B
- ↑ "* zet Cen". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+zet+Cen.
- ↑ Kunitzsch, P.; Smart, T. (2006), A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd revised ed.), Cambridge, Massachusetts: Sky Pub, p. 4, ISBN 978-1-931559-44-7
- ↑ ibid., p.28.
- ↑ (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN:978-986-7332-25-7.
- ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 25 日
- ↑ van Rensbergen, W.; De Loore, C.; Jansen, K. (February 2006), "Evolution of interacting binaries with a B type primary at birth", Astronomy and Astrophysics 446 (3): 1071–1079, doi:10.1051/0004-6361:20053543, Bibcode: 2006A&A...446.1071V
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