Lambda Centauri
 | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 11h 35m 46.88530s[1] |
| Declination | −63° 01′ 11.4313″[1] |
| Apparent magnitude (V) | +3.13[2] |
| Characteristics | |
| Spectral type | B9 III[3][4] |
| U−B color index | −0.19[2] |
| B−V color index | −0.04[2] |
| Astrometry | |
| Radial velocity (Rv) | −1.4[5] km/s |
| Proper motion (μ) | RA: −33.41[1] mas/yr Dec.: −7.08[1] mas/yr |
| Parallax (π) | 7.77 ± 0.34 mas[1] |
| Distance | 420 ± 20 ly (129 ± 6 pc) |
| Details | |
| Mass | 4.5 M☉ |
| Radius | 5.5[6] R☉ |
| Luminosity | 955 L☉ |
| Surface gravity (log g) | 3.04 cgs |
| Temperature | 9,880[7] K |
| Rotational velocity (v sin i) | 183[8] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Lambda Centauri (λ Cen, λ Centauri) is a star in the southern circumpolar constellation of Centaurus. It has an apparent visual magnitude of +3.13,[2] which is bright enough to be seen with the naked eye from the southern hemisphere and places it among the brighter members of this constellation. The star is close enough that its distance can be determined directly using the parallax technique, which gives a value of roughly 420 light-years (130 parsecs) from Earth, with a 5% margin of error.[1] Although a putative solitary star, it has a candidate proper motion companion at an angular separation of 0.73 arcseconds along a position angle of 135°.[9] The nebula IC 2944 lies nearby.
λ Centauri is a B-type giant[10] star with a stellar classification of B9 III.[3] (Although it has also been classified as A1 III.)[7] It has about 5.5[6] times the radius of the Sun and is rotating rapidly with a projected rotational velocity of 183 km s–1.[8] The star's outer atmosphere has an effective temperature of 9,880 K,[7] giving it a blue-white hue.
Based upon the position and movement of this star through space, it is a likely member of the Gould Belt. In particular, it belongs to the Lower Centaurus-Crux (LCC) group of the Scorpius-Centaurus Association, which is the nearest OB association to the Sun. This is a loose grouping of stars that share a common motion through space and therefore formed in the same molecular cloud. The LCC group has an estimated age of 16–20 million years and is centered around a mean distance of 380 light-years (120 parsecs) from Earth.[11]
References
- ^ a b c d e f 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
- ^ a b c d Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99), Bibcode:1966CoLPL...4...99J
- ^ a b Houk, Nancy (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H
- ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ Evans, D. S. (June 20–24, 1966), Batten, Alan Henry; Heard, John Frederick (eds.), The Revision of the General Catalogue of Radial Velocities, University of Toronto: International Astronomical Union, Bibcode:1967IAUS...30...57E
{{citation}}: Unknown parameter|booktitle=ignored (help) - ^ a b Underhill, A. B.; et al. (November 1979), "Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars", Monthly Notices of the Royal Astronomical Society, 189: 601–605, Bibcode:1979MNRAS.189..601U
- ^ a b c Zorec, J.; et al. (July 2009), "Fundamental parameters of B supergiants from the BCD system. I. Calibration of the (λ_1, D) parameters into Teff", Astronomy and Astrophysics, 501 (1): 297–320, Bibcode:2009A&A...501..297Z, doi:10.1051/0004-6361/200811147
- ^ a b Royer, F.; et al. (October 2002), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy and Astrophysics, 393: 897–911, arXiv:astro-ph/0205255, Bibcode:2002A&A...393..897R, doi:10.1051/0004-6361:20020943
- ^ Shatsky, N.; Tokovinin, A. (January 2002), "The mass ratio distribution of B-type visual binaries in the Sco OB2 association", Astronomy and Astrophysics, 382: 92–103, arXiv:astro-ph/0109456, Bibcode:2002A&A...382...92S, doi:10.1051/0004-6361:20011542
- ^ O'Meara, Stephen James (2002), The Caldwell Objects, Cambridge University Press, pp. 399–400, ISBN 0-521-82796-5
- ^ Bobylev, V. V.; Bajkova, A. T. (September 2007), "Kinematics of the Scorpius-Centaurus OB association", Astronomy Letters, 33 (9): 571–583, arXiv:0708.0943, Bibcode:2007AstL...33..571B, doi:10.1134/S1063773707090010
