HD 102776

Last updated
j Centauri
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
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 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 km, 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]

Related Research Articles

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Upsilon2 Centauri is a binary star system in the southern constellation Centaurus. It is visible to the naked eye with an apparent visual magnitude of +4.33. Based upon an annual parallax shift of just 2.57 mas as seen from Earth, this star is located roughly 1,300 light years from the Sun. Relative to its neighbors, the system has a peculiar velocity of 39.2+8.8
−15.2 km/s and it may form a runaway star system.

N Centauri is a binary star in the southern constellation of Centaurus. The brighter star is dimly visible to the naked eye with an apparent visual magnitude of 5.26, and it is approximately 304 light years away based on parallax. It has an absolute magnitude of +0.76 and is drifting further away from the Sun with a radial velocity of +27 km/s. It is a candidate member of the Sco OB2 moving group.

HD 125288 is a single star in the southern constellation of Centaurus. It has the Bayer designation v Centauri ; while HD 125288 is the star's identifier in the Henry Draper catalogue. The object has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.30. Based on parallax measurements, it is located at a distance of approximately 1,230 light years from the Sun. This is a candidate runaway star that is moving to the west and falling back into the Galactic plane. It has an absolute magnitude of −3.56.

3 Centauri is a triple star system in the southern constellation of Centaurus, located approximately 300 light years from the Sun. It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.32. As of 2017, the two visible components had an angular separation of 7.851″ along a position angle of 106°. The system has the Bayer designation k Centauri; 3 Centauri is the Flamsteed designation. It is a suspected eclipsing binary with a variable star designation V983 Centauri.

HD 113703, also known by the Bayer designation f Centauri, is a multiple star system in the southern constellation of Centaurus. The combined apparent visual magnitude of this system is +4.71, which is sufficient to make it faintly visible to the naked eye. The distance to this system is approximately 400 light years based on parallax measurements. It is a member of the Lower Centaurus Crux subgroup of the Scorpius–Centaurus association.

G Centauri is a single star in the southern constellation of Centaurus. It is visible to the naked eye as a faint, blue-white hued star with an apparent visual magnitude of +4.82. This object is located approximately 450 light years from the Sun, based on parallax. It is a member of the Lower Centaurus–Crux group of the Scorpius–Centaurus association, with the former having an age of about 17 million years.

HD 111597 is a suspected astrometric binary star system in the southern constellation of Centaurus. It has the Bayer designation p Centauri, while HD 111597 is the star's identifier from the Henry Draper catalogue. The system is visible to the naked eye as a faint point of light with an apparent visual magnitude of 4.90. It is located at a distance of approximately 380 light years from the Sun based on parallax, and has an absolute magnitude of −0.53. The system is a probable member of the Sco OB2 association of co-moving stars. The visible component is a B-type main-sequence star with a stellar classification of B9V.

1 Scorpii, or b Scorpii, is a single star in the southern zodiac constellation of Scorpius. It has an apparent magnitude of 4.63, which is bright enough to be faintly visible to the naked eye on a dark night. The star shows an annual parallax shift of 6.59 mas from Earth's orbit, which equates to a distance of roughly 490 light years. It is a probable member of the Sco OB2 moving group.

HD 102350 is a single star in the constellation Centaurus. It has a yellow hue and is visible to the naked eye with an apparent visual magnitude of 4.11. The distance to this star is approximately 390 light years based on parallax, but it is drifting closer with a radial velocity of −3 km/s. It has an absolute magnitude of −1.51.

η Lupi, often Latinised as Eta Lupi, is a probable triple star system in the southern constellation of Lupus. It is visible to the naked eye with an apparent visual magnitude of 3.41. Based upon an annual parallax shift of 27.80 mas as seen from Earth, it is located around 136 parsecs (440 ly) distant from the Sun. It is a member of the Upper Centaurus–Lupus subgroup of the nearby Sco OB2 association.

Theta Lupi, Latinized from θ Lupi, is a solitary star in the southern constellation of Lupus. It is visible to the naked eye with an apparent visual magnitude of 4.22. Based upon an annual parallax shift of 7.87 mas as seen from Earth, it is located roughly 410 light years away from the Sun. Relative to its neighbors, this star has a peculiar velocity of 16.7±3.7 km/s. It is a member of the nearby Sco OB2 association.

Phi2 Lupi, Latinized from φ2 Lupi, is a solitary star in the southern constellation of Lupus. With an apparent magnitude of 4.535, it is bright enough to be seen with the naked eye. Based upon an annual parallax shift of 6.28 mas as seen from Earth, it is located around 520 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.052±0.013 due to interstellar dust. It is a member of the Upper Centaurus–Lupus subgroup of the Scorpius–Centaurus association.

<span class="mw-page-title-main">KT Lupi</span> Visual binary star system in the constellation of Lupus

KT Lupi is a visual binary star system in the constellation Lupus. It is visible to the naked eye with a combined apparent visual magnitude of 4.55. As of 1983, the pair had an angular separation of 2.19″±0.03″. Based upon an annual parallax shift of 7.6 mas as seen from Earth's orbit, it is located 430 light-years from the Sun. The system is moving further from the Earth with a heliocentric radial velocity of +6.5 km/s. It is a member of the Lower Centaurus–Crux sub-group of the Scorpius–Centaurus association.

Tau<sup>1</sup> Lupi Star in the constellation Lupus

Tau1 Lupi, Latinized from τ1 Lupi, is a solitary star in the southern constellation of Lupus. It is visible to the naked eye with an apparent visual magnitude of 4.5. Based upon an annual parallax shift of only 2.99 mas as seen from Earth, it is located about 1,090 light years from the Sun. Tau1 Lupi may be a runaway star having a peculiar velocity of 32.6±3.6 km/s. It is a member of the Upper Centaurus–Lupus sub-group of the nearby Sco OB2 association.

HD 134687 is a binary star system in the southern constellation Lupus. It is visible to the naked eye with an apparent visual magnitude of 4.81. The distance to HD 134687 can be estimated from its annual parallax shift of 7.6 mas, yielding roughly 430 light years. It is a member of the ~11 million year old Upper Centaurus–Lupus subgroup of the Scorpius–Centaurus association, the closest OB association to the Sun.

HD 143699 is a single star in the southern constellation of Lupus. It is a dim star but visible to the naked eye with an apparent visual magnitude of 4.90. Based upon an annual parallax shift of 9.2 mas, it is located around 350 light years away. It is most likely a member of the Upper Centaurus–Lupus subgroup of the Sco OB2 moving group.

<span class="mw-page-title-main">N Scorpii</span> Star in the constellation of Scorpius

N Scorpii, also known as HD 148703, is a solitary, bluish-white hued star located in the southern constellation Scorpius. It has an apparent magnitude of 4.23, making it readily visible to the naked eye. N Scorpii was initially given the Bayer designation Alpha Normae by Lacaille but it was later moved from Norma to Scorpius. N Scorpii is currently located 550 light years away based on parallax measurements from the Hipparcos satellite and is part of the Upper Scorpius–Centaurus region of the Scorpius–Centaurus association.

<span class="mw-page-title-main">V1073 Scorpii</span> Variable star in the constellation Scorpius

V1073 Scorpii is a variable star in the constellation Scorpius. It has a non-Greek Bayer designation of k Scorpii. The star has a blue-white hue and is visible to the naked eye with an apparent visual magnitude that fluctuates around +4.87. Parallax measurements yield a distance estimate of approximately 2,920 ly (896 pc) from the Sun, and it is drifting further away with a radial velocity of +7 km/s. It has an absolute magnitude of −6.8

Xi<sup>1</sup> Lupi Probable binary star system in the constellation Lupus

Xi1 Lupi (ξ1 Lup, ξ1 Lupi) is a probable binary star in the southern constellation of Lupus. It is faintly visible to the naked eye with an apparent visual magnitude of 5.1, and forms a visual double star with Xi2 Lupi. Based upon an annual parallax shift of 23.60 mas as seen from Earth, it is located around 140 light-years from the Sun. It is a member of the Upper Scorpius sub-group of the nearby Sco OB2 association.

References

  1. 1 2 3 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.
  2. 1 2 3 4 5 6 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. S2CID   119257644.
  3. 1 2 3 "NSV 5357". Variable Star Index. American Association of Variable Star Observers. Retrieved 2020-02-19.
  4. 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.
  5. 1 2 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. S2CID   18759600. Vizier catalog entry
  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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