HD 102776

Last updated
HD 102776
HD102776LightCurve.png
A light curve for HD 102776, plotted from Hipparcos data [1]
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Centaurus [2]
Right ascension 11h 49m 41.06733s [3]
Declination −63° 47′ 18.5007″ [3]
Apparent magnitude  (V)4.30 [2] (+4.30 - 4.39) [4]
Characteristics
Evolutionary stage main sequence [3]
Spectral type B3V [5]
U−B color index −0.59
B−V color index −0.15
Variable type γ Cas [4]
Astrometry
Radial velocity (Rv)+29.0±4.1 [2] km/s
Proper motion (μ)RA: −22.022 [3] mas/yr
Dec.: +2.755 [3] mas/yr
Parallax (π)4.5957±0.3290  mas [3]
Distance 710 ± 50  ly
(220 ± 20  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
j Cen, NSV 5357, CPD−63°1988, FK5 2944, GC 16201, HD 102776, HIP 57669, HR 4537, SAO 251602 [9]
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 710  light years based on parallax, [3] 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, [5] 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 km/s, 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. [4]

References

  1. ↑ EAS (1997). "The HIPPARCOS and TYCHO catalogues". Astrometric and Photometric Star Catalogues Derived from the ESA Hipparcos Space Astrometry Mission. ESA SP Series. 1200. Noordwijk, Netherlands: ESA Publications Division. Bibcode:1997ESASP1200.....E. ISBN   9290923997 . Retrieved 23 September 2024.
  2. 1 2 3 4 5 6 7 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. XHIP record for this object at VizieR.
  3. 1 2 3 4 5 6 7 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  4. 1 2 3 "NSV 5357". Variable Star Index. American Association of Variable Star Observers. Retrieved 2020-02-19.
  5. 1 2 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.
  6. ↑ 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. S2CID   119491061.
  7. 1 2 3 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.
  8. 1 2 3 4 5 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 .
  9. ↑ "j Cen". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2021-01-28.
  10. ↑ 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 . S2CID   14878976.
  11. ↑ 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.
  12. ↑ 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 (2): 49–77. arXiv: astro-ph/0010057 . Bibcode:2001A&A...365...49H. doi:10.1051/0004-6361:20000014. S2CID   18970167.
  13. ↑ 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.
  14. ↑ 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 . S2CID   119418279. 48.
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