32 Orionis

In today's article we are going to talk about 32 Orionis, a topic that has captured the attention of many in recent times. 32 Orionis is a very broad and relevant topic in today's society, since it has an impact on various areas of daily life. In this article we will explore the different aspects related to 32 Orionis, from its origin and evolution to its influence on culture and people's lives. In addition, we will analyze its importance in the current context and how it has set a trend in different areas. We are sure that this article will provide you with valuable information and help you better understand the relevance and impact of 32 Orionis in today's society.

32 Orionis
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]
Distance300 ± 20 ly
(93 ± 6 pc)
Absolute magnitude (MV)–0.63[5]
Details
32 Ori A
Mass5.0[6] M☉
Radius2.9[7] R☉
Luminosity388[5] L☉
Surface gravity (log g)4.40[8] cgs
Temperature16,020[9] K
Rotational velocity (v sin i)169[8] km/s
Age65[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
SIMBADdata

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] Research in 2015 suggested that Bellatrix is a probable member of the group due to its distance and position in the sky and suggested it be called the Bellatrix Cluster,[12] although further research in 2017 called Bellatrix's membership into question due to its proper motion deviating significantly from the group.[11]

The primary component of this system is a B-type main-sequence star with a stellar classification of B5V[13] 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.[14] 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.[15]

References

  1. ^ a b c d e f 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. ^ a b c d 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. ^ a b c d 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. ^ a b 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. ^ a b 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. ^ a b c 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. ^ a b 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. ^ Bouy, H.; Alves, J. (2015-12-01). "Cosmography of OB stars in the solar neighbourhood". Astronomy & Astrophysics. 584: A26. Bibcode:2015A&A...584A..26B. doi:10.1051/0004-6361/201527058. ISSN 0004-6361.
  13. ^ Hoffleit, D.; Warren, W. H. (1995). "Bright Star Catalogue". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H. 5050 (5th ed.). Bibcode:1995yCat.5050....0H.
  14. ^ 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.
  15. ^ 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