32 Orionis

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32 Orionis
Orion constellation map.svg
Red circle.svg
Location of 32 Orionis (circled)
Observation data
Epoch J2000       Equinox J2000
Constellation Orion
Right ascension 05h 30m 47.05091s [1]
Declination +05° 56′ 53.2925″ [1]
Apparent magnitude  (V)4.20 [2] (4.43 + 5.80) [3]
Characteristics
Spectral type B5V + ? + B7V [3]
U−B color index –0.56 [2]
B−V color index –0.13 [2]
Astrometry
Radial velocity (Rv)+18.60 [4]  km/s
Proper motion (μ)RA: +5.10 [1]   mas/yr
Dec.: –33.30 [1]   mas/yr
Parallax (π)10.77 ± 0.64  mas [1]
Distance 300 ± 20  ly
(93 ± 6  pc)
Absolute magnitude  (MV)–0.63 [5]
Details
32 Ori A
Mass 5.0 [6]   M☉
Radius 2.9 [7]   R☉
Luminosity 388 [5]   L☉
Surface gravity (log g)4.40 [8]   cgs
Temperature 16,020 [9]   K
Rotational velocity (v sin i)169 [8]  km/s
Age 65 [8]   Myr
Other designations
A Ori, 32 Ori, NSV  14617, BD+05°939, GC  6813, HD  36267, HIP  25813, HR  1839, SAO  112849, CCDM J05308+0557AB, WDS J05308+0557AB [10]
Database references
SIMBAD data

32 Orionis is a triple [3] star system in the equatorial constellation of Orion. It has the Bayer designation A Orionis, while 32 Orionis is the Flamsteed designation. This system is visible to the naked eye as a faint point of light with a combined apparent visual magnitude of 4.20. [2] It is located approximately 303  light-years away from the Sun based on parallax, [1] and is drifting further away with a radial velocity of +18.6 km/s. [4]

The system is a member of the eponymous 32 Orionis group, a young, nearby association of 46 co-moving stars first discovered in 2007. [11]

The primary component of this system is a B-type main-sequence star with a stellar classification of B5V [12] and a magnitude around 4.43. This is actually a spectroscopic binary with an orbital period of 3.964 days and eccentricity of 0.38. [3] The unseen companion has an estimated mass of 0.6 times that of the Sun. [13] Component B, at an angular separation of 1.08″ from the primary, is a class B7V star with a magnitude of 5.8, orbiting with the primary at a period of 614 years and eccentricity 0.22. [14]

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References

  1. 1 2 3 4 5 6 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 Ducati, J. R. (2002). "Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. 1 2 3 4 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.
  4. 1 2 Kharchenko, N.V.; et al. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten. 328 (9): 889. arXiv: 0705.0878 . Bibcode:2007AN....328..889K. doi:10.1002/asna.200710776. S2CID   119323941.
  5. 1 2 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. Vizier catalog entry
  6. ↑ Tetzlaff, N.; et al. (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. Vizier catalog entry
  7. ↑ Allende Prieto, C.; Lambert, D. L. (1999). "Fundamental parameters of nearby stars from the comparison with evolutionary calculations: Masses, radii and effective temperatures". Astronomy and Astrophysics. 352: 555–562. arXiv: astro-ph/9911002 . Bibcode:1999A&A...352..555A. Vizier catalog entry
  8. 1 2 3 David, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv: 1501.03154 . Bibcode:2015ApJ...804..146D. doi:10.1088/0004-637X/804/2/146. S2CID   33401607. Vizier catalog entry
  9. ↑ Zorec, J.; et al. (2009). "Fundamental parameters of B supergiants from the BCD system". Astronomy and Astrophysics. 501 (1): 297–320. arXiv: 0903.5134 . Bibcode:2009A&A...501..297Z. doi:10.1051/0004-6361/200811147. S2CID   14969137.
  10. ↑ "32 Ori". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2019-07-10.
  11. ↑ Bell, Cameron P. M.; et al. (June 2017). "A stellar census of the nearby, young 32 Orionis group". Monthly Notices of the Royal Astronomical Society. 468 (1): 1198–1220. arXiv: 1703.00015 . Bibcode:2017MNRAS.468.1198B. doi:10.1093/mnras/stx535.
  12. ↑ Hoffleit, D.; Warren, W. H. (1995). "Bright Star Catalogue". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H (5th ed.). 5050. Bibcode:1995yCat.5050....0H.
  13. ↑ Tokovinin, A. (2008). "Comparative statistics and origin of triple and quadruple stars". Monthly Notices of the Royal Astronomical Society. 389 (2): 925–938. arXiv: 0806.3263 . Bibcode:2008MNRAS.389..925T. doi:10.1111/j.1365-2966.2008.13613.x. S2CID   16452670.
  14. ↑ Malkov, O. Yu.; Tamazian, V. S.; Docobo, J. A.; Chulkov, D. A. (2012). "Dynamical masses of a selected sample of orbital binaries". Astronomy & Astrophysics. 546: A69. Bibcode:2012A&A...546A..69M. doi: 10.1051/0004-6361/201219774 . Vizier catalog entry
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