Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Scorpius |
Right ascension | 17h 18m 23.06137s [2] |
Declination | −34° 24′ 30.6308″ [2] |
Apparent magnitude (V) | 9.27 [3] |
Characteristics | |
Evolutionary stage | Wolf-Rayet star |
Spectral type | WC7 + B0III [4] |
Apparent magnitude (J) | 7.436 [5] |
Apparent magnitude (K) | 6.666 [6] |
U−B color index | −0.07 [7] |
B−V color index | +0.63 [7] |
Variable type | β Cep [3] |
Astrometry | |
Proper motion (μ) |
RA: −0.92
[2]
mas/
yr Dec.: −4.80 [2] mas/ yr |
Parallax (π) | 1.84 ± 1.62 mas [2] |
Distance | 2,100 ± 800 [4] pc |
Absolute magnitude (MV) | −4.3 + −4.3 [4] |
Details | |
WR | |
Radius | 10 [8] R☉ |
Luminosity | 200,000 [4] [8] L☉ |
Temperature | 56,000 [8] K |
B | |
Mass | 19 M☉ |
Radius | ~8.5 (SBL) R☉ |
Luminosity | 63,000 [4] L☉ |
Temperature | 31,405 [4] K |
Age | 4.0 [4] Myr |
Other designations | |
Database references | |
SIMBAD | data |
WR 86 is a visual binary in the constellation Scorpius consisting of a Wolf-Rayet star and a β Cephei variable. It lies 2° west of NGC 6357 on the edge of the Great Rift in the Milky Way in the tail of the Scorpion.
WR 86 is a binary with two components of equal visual brightness 0.3" apart. [9] One has the emission-line spectrum of a WC7 Wolf-Rayet star, while the other is a B0 giant. The blue giant varies slightly in brightness every 3.5 hours. The WR star may also be slightly variable. [4]
The pulsations of the B-type giant are characteristic of a β Cephei variable. Analysis of its pulsations and comparison to the expected properties of a WC7 star suggest that both stars could have evolved without mass exchange. The WR and B stars would have had initial masses of 40 M☉ and 20 M☉ respectively four million years ago. [4]
Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Scorpius |
Right ascension | 17h 18m 23.06137s [2] |
Declination | −34° 24′ 30.6308″ [2] |
Apparent magnitude (V) | 9.27 [3] |
Characteristics | |
Evolutionary stage | Wolf-Rayet star |
Spectral type | WC7 + B0III [4] |
Apparent magnitude (J) | 7.436 [5] |
Apparent magnitude (K) | 6.666 [6] |
U−B color index | −0.07 [7] |
B−V color index | +0.63 [7] |
Variable type | β Cep [3] |
Astrometry | |
Proper motion (μ) |
RA: −0.92
[2]
mas/
yr Dec.: −4.80 [2] mas/ yr |
Parallax (π) | 1.84 ± 1.62 mas [2] |
Distance | 2,100 ± 800 [4] pc |
Absolute magnitude (MV) | −4.3 + −4.3 [4] |
Details | |
WR | |
Radius | 10 [8] R☉ |
Luminosity | 200,000 [4] [8] L☉ |
Temperature | 56,000 [8] K |
B | |
Mass | 19 M☉ |
Radius | ~8.5 (SBL) R☉ |
Luminosity | 63,000 [4] L☉ |
Temperature | 31,405 [4] K |
Age | 4.0 [4] Myr |
Other designations | |
Database references | |
SIMBAD | data |
WR 86 is a visual binary in the constellation Scorpius consisting of a Wolf-Rayet star and a β Cephei variable. It lies 2° west of NGC 6357 on the edge of the Great Rift in the Milky Way in the tail of the Scorpion.
WR 86 is a binary with two components of equal visual brightness 0.3" apart. [9] One has the emission-line spectrum of a WC7 Wolf-Rayet star, while the other is a B0 giant. The blue giant varies slightly in brightness every 3.5 hours. The WR star may also be slightly variable. [4]
The pulsations of the B-type giant are characteristic of a β Cephei variable. Analysis of its pulsations and comparison to the expected properties of a WC7 star suggest that both stars could have evolved without mass exchange. The WR and B stars would have had initial masses of 40 M☉ and 20 M☉ respectively four million years ago. [4]