3 Centauri

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3 Centauri
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Centaurus
Right ascension 13h 51m 49.60s [1]
Declination −32° 59′ 38.7″ [1]
Apparent magnitude  (V)4.32 [2] (4.52 + 5.97) [3]
Characteristics
Spectral type B5 III-IVp [4] + B8 V [5]
B−V color index −0.146±0.003 [2]
Variable type Eclipsing? [6]
Astrometry
Radial velocity (Rv)+7.5±1.6 [7]  km/s
Absolute magnitude  (MV)−0.46 [2]
A
Proper motion (μ)RA: −34.698±0.864 [8]   mas/yr
Dec.: −27.909±0.792 [8]   mas/yr
Parallax (π)11.0982 ± 0.4267  mas
Distance 290 ± 10  ly
(90 ± 3  pc)
B
Proper motion (μ)RA: −36.737±0.266 [9]   mas/yr
Dec.: −23.774±0.189 [9]   mas/yr
Parallax (π)10.2659 ± 0.1380  mas [9]
Distance 318 ± 4  ly
(97 ± 1  pc)
Orbit [10]
PrimaryBa
CompanionBb
Period (P)17.428 d
Eccentricity (e)0.21
Periastron epoch (T)2443296.44 JD
Argument of periastron (ω)
(secondary)		15°
Semi-amplitude (K1)
(primary)		17 km/s
Details
3 Cen A
Mass 5.0±0.1 [11]   M☉
Surface gravity (log g)3.80 [12]   cgs
Temperature 17,500 [12]   K
Age 47.4±7.3 [11]   Myr
3 Cen B
Mass 2.47±0.10 [5]   M☉
Radius 2.8 [13]   R☉
Luminosity50.2+11.7
−9.5 [5]   L☉
Temperature 9,638+67
−66 [5]   K
Rotational velocity (v sin i)135 [5]  km/s
Other designations
k Centauri, 3 Cen, V983 Centauri, HIP  67669, WDS J13518-3300 [14]
3 Cen A: GC  18724, HD  120709, HR  5210, SAO  204916
3 Cen B: GC  18725, HD  120710, HR  5211, SAO  204917
Database references
SIMBAD data
A
B

3 Centauri is a triple star [3] system in the southern constellation of Centaurus, [14] located approximately 300 light years from the Sun. [8] [9] It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.32. [2] As of 2017, the two visible components had an angular separation of 7.851″ along a position angle of 106°. [3] 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. [6]

The brighter member, designated component A, is a magnitude 4.52 [3] chemically peculiar star of the helium-weak (CP4) variety, and has a stellar classification of B5 III-IVp. [4] The spectrum of the star displays overabundances of elements such as nitrogen, phosphorus, manganese, iron, and nickel, while carbon, oxygen, magnesium, aluminium, sulfur, and chlorine appear underabundant relative to the Sun. [12] Weak emission line features are also visible. [15]

The magnitude 5.97 [3] secondary, component B, is a single-lined spectroscopic binary star system with an orbital period of 17.4 days and an eccentricity of 0.21. [10] The pair have an angular separation of 2.485  mas . The visible component is a B-type main-sequence star with a class of B8 V. [5]

Related Research Articles

17 Aquarii, abbreviated 17 Aqr, is a spectroscopic binary star system in the constellation of Aquarius. 17 Aquarii is the Flamsteed designation. It appears to the naked eye as a faint sixth magnitude star, having a combined apparent visual magnitude of 5.99. The distance to 17 Aqr can be estimated from its annual parallax shift of 4.9 mas, which yields a separation of around 660 light years. It is moving further away with a heliocentric radial velocity of 18 km/s.

<span class="mw-page-title-main">4 Cassiopeiae</span> Star in the constellation Cassiopeia

4 Cassiopeiae is a red giant in the northern constellation of Cassiopeia, located approximately 790 light-years away from the Sun. It is visible to the naked eye as a faint, red-hued star with a baseline apparent visual magnitude of 4.96. At the distance of this system, its visual magnitude is diminished by an extinction of 0.56 due to interstellar dust. This system is moving closer to the Earth with a heliocentric radial velocity of −39 km/s.

<span class="mw-page-title-main">Lambda Centauri</span> Star in the constellation Centaurus

Lambda Centauri, Latinized from λ Centauri, is a star in the southern circumpolar constellation of Centaurus. It has an apparent visual magnitude of +3.13, 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 approximately 470 light-years from the Sun. 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°. The nebula IC 2944 lies nearby.

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.

D Centauri is a double star in the southern constellation of Centaurus. The system is faintly visible to the naked eye as a point of light with a combined apparent magnitude of +5.31; the two components are of magnitude 5.78 and 6.98, respectively. It is located at a distance of approximately 610 light years from the Sun based on parallax, and is drifting further away with a radial velocity of ~10 km/s.

<span class="mw-page-title-main">Rho Centauri</span> Binary star system in the constellation Centaurus

Rho Centauri, Latinized from ρ Centauri, is a binary star system in the southern constellation of Centaurus. It is visible to the naked eye as a blue-white hued point of light with a combined apparent visual magnitude of +3.97. The system is located approximately 276 light years from the Sun based on parallax, and is drifting further away with a radial velocity of around +15 km/s. It is a proper motion member of the Lower Centaurus–Crux sub-group in the Scorpius–Centaurus OB association, the nearest such association of co-moving massive stars to the Sun.

1 Centauri, or i Centauri, is a yellow-white-hued binary star system in the southern constellation Centaurus. It can be seen with the naked eye, having an apparent visual magnitude of +4.23. Based upon an annual parallax shift of 51.54 mas as seen from Earth's orbit, it is located 51.5 light-years from the Sun. The system is moving closer to the Sun with a radial velocity of −21.5 km/s.

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 102776, also known by its Bayer designation j Centauri, is a suspected astrometric binary 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. 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. It is a member of the Lower Centaurus Crux subgroup of the Sco OB2 association. 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.

HD 111915 is a single star in the southern constellation of Centaurus. It has the Bayer designation e Centauri, while HD 111915 is the star's identifier in the Henry Draper Catalogue. This is an aging giant star with a stellar classification of K3-4III. It is faintly visible to the naked eye with an apparent visual magnitude of +4.33. The distance to this star is approximately 294 light years based on parallax.

HD 116243 is a single star in the southern constellation of Centaurus. It has the Bayer designation m Centauri, while HD 116243 is the identifier from the Henry Draper catalogue. This star has a yellow hue and is faintly visible to the naked eye with an apparent visual magnitude of +4.52. It is located at a distance of approximately 244 light years from the Sun based on parallax, and it has an absolute magnitude of 0.01. It is drifting further away with a radial velocity of +13.3 km/s.

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.

K Centauri is a possible binary star in the southern constellation of Centaurus. It has a white hue and is bright enough to be visible to the naked eye, having an apparent visual magnitude of +5.04.

<span class="mw-page-title-main">V Centauri</span> Variable star in the constellation Centaurus

V Centauri is a Classical Cepheid variable, a type of variable star, in the constellation Centaurus. It is approximately 2,350 light-years away based on parallax.

HD 224635 and HD 224636 is a pair of stars comprising a binary star system in the constellation Andromeda. They are located approximately 94 light years away and they orbit each other every 717 years.

26 Vulpeculae is a close binary star system in the northern constellation of Vulpecula, around 644 light years away from the Sun. It is a challenge to view with the naked eye, having an apparent visual magnitude of 6.40. The star is moving closer to the Earth with a heliocentric radial velocity of −63 km/s, and is expected to come within 225 light-years in around 2.6 million years.

HD 137058 is a star in the southern constellation of Lupus. Eggleton and Tokovinin (2008) list it as a single star, although Nitschelm and David (2011) noted it may be a double-lined spectroscopic binary. Its apparent visual magnitude is 4.60, which is bright enough to be visible to the naked eye. Based upon an annual parallax shift of 13.6 mas, it is located 240 light years away.

23 Orionis is a double star located around 1,200 light-years away from the Sun in the equatorial constellation of Orion. It is visible to the naked eye as a dim, blue-white-hued point of light with a combined apparent visual magnitude of 4.99. The pair are moving away from the Earth with a heliocentric radial velocity of +18 km/s, and they are members of the Orion OB1 association, subgroup 1a.

<span class="mw-page-title-main">HD 21278</span> Binary star system in the constellation Perseus

HD 21278 is a binary star system in the constellation Perseus, located within the 60±7 million year old Alpha Persei Cluster. It has a blue-white hue and is visible to the naked eye with a combined apparent visual magnitude of 4.99. The system is located at a distance of approximately 580 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +1.20 km/s.

<span class="mw-page-title-main">Y Centauri</span> Variable star in the constellation Centaurus

Y Centauri or Y Cen is a semiregular variable star in the constellation of Centaurus.

References

  1. 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
  2. 1 2 3 4 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 4 5 Veramendi, M. E.; González, J. F. (March 2014). "Spectroscopic study of early-type multiple stellar systems. I. Orbits of spectroscopic binary subsystems". Astronomy & Astrophysics. 563: 15. Bibcode:2014A&A...563A.138V. doi: 10.1051/0004-6361/201322840 . hdl: 11336/4892 . A138.
  4. 1 2 Sigut, T. A. A.; et al. (February 2000). "Emission Lines in the Spectrum of the 3HE Star 3 Centauri A". The Astrophysical Journal. 530 (2): L89–L92. arXiv: astro-ph/0001090 . Bibcode:2000ApJ...530L..89S. doi:10.1086/312499. PMID   10655172. S2CID   30530913.
  5. 1 2 3 4 5 6 Zorec, J.; Royer, F. (2012). "Rotational velocities of A-type stars. IV. Evolution of rotational velocities". Astronomy & Astrophysics. 537: A120. arXiv: 1201.2052 . Bibcode:2012A&A...537A.120Z. doi:10.1051/0004-6361/201117691. S2CID   55586789.
  6. 1 2 Samus, N. N.; et al. (2017). "General Catalogue of Variable Stars". Astronomy Reports. 5.1. 61 (1): 80–88. Bibcode:2017ARep...61...80S. doi:10.1134/S1063772917010085. S2CID   125853869.
  7. ↑ Gontcharov, G. A. (November 2006). "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID   119231169.
  8. 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.
  9. 1 2 3 4 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.
  10. 1 2 Pourbaix, D.; et al. (2004). "SB9: The Ninth Catalogue of Spectroscopic Binary Orbits". Astronomy & Astrophysics. 424: 727–732. arXiv: astro-ph/0406573 . Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213. S2CID   119387088.
  11. 1 2 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.
  12. 1 2 3 Sadakane, Kozo; Nishimura, Masayoshi (June 2018). "Spectroscopic abundance analyses of the 3He stars HD 185330 and 3 Cen A". Publications of the Astronomical Society of Japan. 70 (3): 40. arXiv: 1802.10087 . Bibcode:2018PASJ...70...40S. doi:10.1093/pasj/psy031. 40.
  13. ↑ Pasinetti Fracassini, L. E.; Pastori, L.; Covino, S.; Pozzi, A. (February 2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)". Astronomy and Astrophysics (Third ed.). 367: 521–524. arXiv: astro-ph/0012289 . Bibcode:2001A&A...367..521P. doi:10.1051/0004-6361:20000451. S2CID   425754.
  14. 1 2 "3 Cen". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-04-11.
  15. ↑ Wahlgren, G. M.; Hubrig, S. (May 2004). "Emission lines in the optical spectrum of 3 Cen A". Astronomy and Astrophysics. 418 (3): 1073–1081. Bibcode:2004A&A...418.1073W. doi: 10.1051/0004-6361:20034257 .
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