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Binary star system in the constellation Vela From Wikipedia, the free encyclopedia
HD 83058 is a subgiant star in the constellation Vela and a spectroscopic binary. It is visible to the naked eye with an apparent visual magnitude of 5.0. Based upon an annual parallax shift of 3.4254 mas, it is located 950 light-years from the Sun. The system is moving further away with a heliocentric radial velocity of +35 km/s.
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Vela |
Right ascension | 09h 34m 08.793s[1] |
Declination | −51° 15′ 18.95″[1] |
Apparent magnitude (V) | 5.00[2] |
Characteristics | |
Evolutionary stage | subgiant |
Spectral type | B2 IV[3] |
U−B color index | −0.97[2] |
B−V color index | −0.19[2] |
Astrometry | |
Radial velocity (Rv) | +16.5±3.0[4] km/s |
Proper motion (μ) | RA: −130.55[1] mas/yr Dec.: +42.98[1] mas/yr |
Parallax (π) | 3.4252 ± 0.1907 mas[1] |
Distance | 950 ± 50 ly (290 ± 20 pc) |
Absolute magnitude (MV) | −2.84[2] |
Details | |
primary | |
Mass | 9.3[5] M☉ |
Radius | 5.405[6] R☉ |
Luminosity | 2,686[6] L☉ |
Surface gravity (log g) | 3.779[6] cgs |
Temperature | 17,887[6] K |
Rotational velocity (v sin i) | 64±2[4] km/s |
Age | 14.1[5] Myr |
secondary | |
Rotational velocity (v sin i) | 24±2[4] km/s |
Other designations | |
Database references | |
SIMBAD | data |
HD 83058 has generally been considered to be a single star,[8] but high-resolution spectra show it to be a double-lined spectroscopic binary.[9] The two components have approximately the same spectral type.[4] Line-profile variations have been detected which suggest that at least one component pulsates, as is common for stars of this spectral class.[10]
HD 83058 was proposed as a runaway star from a supernova explosion. However, the discovery that it is a binary makes this unlikely.[4]
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