Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Orion |
Right ascension | 05h 37m 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±21 gauss. [3] It also has small (0.11 magnitude) short-period, single-mode pulsations of the Delta Scuti type. [9]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Orion |
Right ascension | 05h 37m 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±21 gauss. [3] It also has small (0.11 magnitude) short-period, single-mode pulsations of the Delta Scuti type. [9]