Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Scorpius |
Right ascension | 17h 06m 53.9045s[2] |
Declination | −42° 36′ 39.704″[2] |
Apparent magnitude (V) | 9.03[3] |
Characteristics | |
Spectral type | WNpec[4] |
U−B color index | -0.19[3] |
B−V color index | 0.84[3] |
Astrometry | |
Proper motion (μ) | RA: +2.545[2] mas/yr Dec.: −2.251[2] mas/yr |
Parallax (π) | 0.6919 ± 0.0193 mas[2] |
Distance | 1,270[5] pc |
Orbit[6] | |
Period (P) | 6.1228 days |
Eccentricity (e) | 0.17 |
Inclination (i) | 45° |
Argument of periastron (ω) (secondary) | 197±14° |
Semi-amplitude (K1) (primary) | 230±12.7 km/s |
Details | |
WN | |
Mass | 5.5[6] M☉ |
Radius | 19.51[a] R☉ |
Luminosity | 80,000[5] L☉ |
Temperature | 22,000[5] K |
O | |
Mass | 29.1[6] M☉ |
Radius | 10[6] R☉ |
Other designations | |
V1104 Scorpii, 2MASS J17065390-4236397 | |
Database references | |
SIMBAD | data |
HD 326823, also known as V1104 Scorpii, is a binary star containing a unique emission-line star, which is in the midst of transitioning to a nitrogen-rich Wolf-Rayet star, as well as being a candidate Luminous blue variable, located 4,142 light years away in the constellation of Scorpius. The primary is very evolved, because it is composed of almost entirely helium, and only 3% of it is still hydrogen,[4] and it has lost most of its mass to the now-very-massive secondary. The underlying mechanisms and mass transfers in the system are comparable to other W Serpentis systems, such as Beta Lyrae and RY Scuti.[4]
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