HD 102776
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 11h 49m 41.05745s[1] |
| Declination | −63° 47′ 18.4299″[1] |
| Apparent magnitude (V) | 4.30[2] (+4.30 - 4.39)[3] |
| Characteristics | |
| Spectral type | B3V[4] |
| U−B color index | −0.59 |
| B−V color index | −0.15 |
| Variable type | γ Cas[3] |
| Astrometry | |
| Radial velocity (Rv) | +29.0±4.1[2] km/s |
| Proper motion (μ) | RA: -20.76 ± 0.56[5] mas/yr Dec.: 4.30 ± 0.48[5] mas/yr |
| Parallax (π) | 5.4391 ± 0.4369 mas[1] |
| Distance | 600 ± 50 ly (180 ± 10 pc) |
| Absolute magnitude (MV) | −1.98[2] |
| Details | |
| Mass | 5.955 M☉[6] 7.2±0.1[7] M☉ |
| Radius | 5.00±0.10[8] R☉ |
| Luminosity | 1,342[2] L☉ |
| Surface gravity (log g) | 3.20±0.03[8] cgs |
| Temperature | 20,000±200[8] K |
| Rotational velocity (v sin i) | 200±4[8] km/s |
| Age | 31.6±0.6[7] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 102776, also known by its Bayer designation j Centauri, is a suspected astrometric binary[10] star system in the southern constellation of Centaurus. It has a blue-white hue and is faintly visible to the naked eye with a typical apparent visual magnitude of 4.30.[2] The distance to this star is approximately 600 light years based on parallax, and it is drifting further away with a radial velocity of ~29 km/s.[2] It is a member of the Lower Centaurus Crux subgroup of the Sco OB2 association.[11] HD 102776 has a relatively large peculiar velocity of 31.1 km/s and is a candidate runaway star that was ejected from its association, most likely by a supernova explosion.[12]
The stellar classification of the visible component is B3V,[4] matching a B-type main-sequence star. It is around 32[7] million years old and is spinning rapidly with estimates of its projected rotational velocity ranging from 200[8] up to 270 kms, giving it an equatorial bulge that is up to 11% larger than the polar radius.[13] This is a Be star showing emission features in its Balmer lines due to a circumstellar disk of decreated gas.[14] It is classified as a suspected Gamma Cassiopeiae type variable star with a visual magnitude varying from +4.30 down to +4.39.[3]
References
- ^ a b c 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 d e f 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.
- ^ a b c "NSV 5357". Variable Star Index. American Association of Variable Star Observers. Retrieved 2020-02-19.
- ^ a b Houk, Nancy (1979). Michigan catalogue of two-dimensional spectral types for the HD stars. Vol. 1. Ann Arbor, Michigan: Department of Astronomy, University of Michigan. Bibcode:1978mcts.book.....H.
- ^ a b van Leeuwen, F. (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. Vizier catalog entry
- ^ Kervella, Pierre; Arenou, Frédéric; Mignard, François; Thévenin, Frédéric (2019). "Stellar and substellar companions of nearby stars from Gaia DR2. Binarity from proper motion anomaly". Astronomy and Astrophysics. 623: A72. arXiv:1811.08902. Bibcode:2019A&A...623A..72K. doi:10.1051/0004-6361/201834371.
- ^ a b c Tetzlaff, N.; et al. (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. arXiv:1007.4883. Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x. S2CID 118629873.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ a b c d e Arcos, C.; et al. (March 2018). "Stellar parameters and H α line profile variability of Be stars in the BeSOS survey". Monthly Notices of the Royal Astronomical Society. 474 (4): 5287–5299. arXiv:1711.08675. Bibcode:2018MNRAS.474.5287A. doi:10.1093/mnras/stx3075.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - ^ "j Cen". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-01-28.
- ^ 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) - ^ Brown, A. G. A.; Verschueren, W. (March 1997). "High S/N Echelle spectroscopy in young stellar groups. II. Rotational velocities of early-type stars in SCO OB2". Astronomy and Astrophysics. 319: 811–838. arXiv:astro-ph/9608089. Bibcode:1997A&A...319..811B.
- ^ Hoogerwerf, R.; et al. (January 2001). "On the origin of the O and B-type stars with high velocities. II. Runaway stars and pulsars ejected from the nearby young stellar groups". Astronomy and Astrophysics. 365: 49–77. arXiv:astro-ph/0010057. Bibcode:2001A&A...365...49H. doi:10.1051/0004-6361:20000014.
- ^ van Belle, Gerard T. (March 2012). "Interferometric observations of rapidly rotating stars". The Astronomy and Astrophysics Review. 20 (1): 51. arXiv:1204.2572. Bibcode:2012A&ARv..20...51V. doi:10.1007/s00159-012-0051-2. S2CID 119273474.
- ^ Arcos, C.; et al. (June 2017). "Evidence for Different Disk Mass Distributions between Early- and Late-type Be Stars in the BeSOS Survey". The Astrophysical Journal. 842 (1): 18. arXiv:1704.08133. Bibcode:2017ApJ...842...48A. doi:10.3847/1538-4357/aa6f5f. 48.
{{cite journal}}: CS1 maint: unflagged free DOI (link)
