05h37m13.2624s, −06° 35′ 00.5654″
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Orion |
| Right ascension | 05h37m 13.2624s[2] |
| Declination | −06° 35′ 00.5654″[2] |
| Apparent magnitude (V) | 9.69 |
| Characteristics | |
| Evolutionary stage | Herbig Ae/Be star |
| Spectral type | A5II-III[3] |
| Apparent magnitude (g) | 10.38 |
| Astrometry | |
| Proper motion (μ) | RA: 0.873±0.025 mas/yr[2] Dec.: 0.654±0.023 mas/yr[2] |
| Parallax (π) | 2.6173 ± 0.0279 mas[2] |
| Distance | 1,250 ± 10 ly (382 ± 4 pc) |
| Details | |
| Mass | 1.85+0.15 −0.00[4] M☉ |
| Radius | 1.59±0.20[4] R☉ |
| Luminosity | 39[5] L☉ |
| Surface gravity (log g) | 3.5[6] cgs |
| Temperature | 8750[6] K |
| Rotational velocity (v sin i) | 37±2[3] km/s |
| Age | 17.14+2.80 −0.00[4] Myr |
| Other designations | |
BD-06 1259, GSC 04778-01087, HIP 26403, 2MASS J05371326-0635005, Gaia DR2 3016930993175537536, Gaia EDR3 3016930993175889792, TYC 4778-1087-1 | |
| Database references | |
| SIMBAD | data |
BF Orionis is a young Herbig Ae/Be star in the constellation of Orion about 1250 light years away, within the Orion Nebula. It is the most massive star of the small birth cluster of four stars.[7]
BF Orionis is a Herbig Ae/Be star variable similar to UX Orionis. It is still accreting mass, producing about 2L☉ through the release of gravitational energy, and is surrounded by a massive, optically thick protoplanetary disk of 0.005±0.002M☉[4] visible nearly edge-on. The brightness of the star is strongly variable, with irregular deep minima down to 13th magnitude. The variations are suspected to be partly caused by a brown dwarf or massive planet embedded in the protoplanetary disk,[1] together with very large comets.[8]
Unlike typical Herbig Ae/Be stars, 90-95% of which do not have detectable magnetic fields, BF Orionis has a fairly strong longitudinal magnetic field of −144±21gauss.[3] It also has small (0.11 magnitude) short-period, single-mode pulsations of the Delta Scuti type.[9]
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