32 Orionis

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]

  1. ^ a b c d e f Cite error: The named reference vanLeeuwen2007 was invoked but never defined (see the help page).
  2. ^ a b c d Cite error: The named reference Ducati2002 was invoked but never defined (see the help page).
  3. ^ a b c d Cite error: The named reference Eggleton2008 was invoked but never defined (see the help page).
  4. ^ a b Cite error: The named reference Kharchenko2007 was invoked but never defined (see the help page).
  5. ^ a b Cite error: The named reference XHIP was invoked but never defined (see the help page).
  6. ^ Cite error: The named reference Tetzlaff2011 was invoked but never defined (see the help page).
  7. ^ Cite error: The named reference AllendePrieto was invoked but never defined (see the help page).
  8. ^ a b c Cite error: The named reference David2015 was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Zorec2009 was invoked but never defined (see the help page).
  10. ^ Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  11. ^ a b Cite error: The named reference Bell2017 was invoked but never defined (see the help page).
  12. ^ Bouy, H.; Alves, J. (2015-12-01). "Cosmography of OB stars in the solar neighbourhood". Astronomy & Astrophysics. 584: A26. doi:10.1051/0004-6361/201527058. ISSN 0004-6361.
  13. ^ Cite error: The named reference Hoffleit1991 was invoked but never defined (see the help page).
  14. ^ Cite error: The named reference Tokovinin2008 was invoked but never defined (see the help page).
  15. ^ Cite error: The named reference Malkov2012 was invoked but never defined (see the help page).