32 Orionis

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]

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]
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

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]