WR 86

WR 86

A light curve for V1035 Scorpii, plotted from TESS data[1]
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]
Distance2,100 ± 800[4] pc
Absolute magnitude (MV)−4.3 + −4.3[4]
Details
WR
Radius10[8] R☉
Luminosity200,000[4][8] L☉
Temperature56,000[8] K
B
Mass19 M☉
Radius~8.5 (SBL) R☉
Luminosity63,000[4] L☉
Temperature31,405[4] K
Age4.0[4] Myr
Other designations
V1035 Scorpii, CD−34°11622, HD 156327, HIP 84655, 2MASS J17182306-3424306, WDS J17184-3425
Database references
SIMBADdata

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]

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