Omicron Puppis
Variable Star in the constellation Puppis / From Wikipedia, the free encyclopedia
Omicron Puppis (ο Puppis) is candidate binary star[6] system in the southern constellation of Puppis. It is visible to the naked eye, having a combined apparent visual magnitude of +4.48.[2] Based upon an annual parallax shift of 2.30 mas as seen from Earth,[1] it is located roughly 1,400 light years from the Sun.
Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Puppis |
Right ascension | 07h 48m 05.16839s[1] |
Declination | −25° 56′ 13.8123″[1] |
Apparent magnitude (V) | +4.48[2] |
Characteristics | |
Spectral type | B1 IVnne[3] |
U−B color index | −1.02[2] |
B−V color index | −0.09[2] |
Variable type | LERI |
Astrometry | |
Radial velocity (Rv) | +15.0[4] km/s |
Proper motion (μ) | RA: −10.09[1] mas/yr Dec.: +4.26[1] mas/yr |
Parallax (π) | 2.30 ± 0.23 mas[1] |
Distance | 1,400 ± 100 ly (430 ± 40 pc) |
Absolute magnitude (MV) | −3.77[5] |
Orbit[6] | |
Period (P) | 28.903±0.004 d |
Eccentricity (e) | 0 |
Periastron epoch (T) | 2456012.93 ± 0.04 |
Semi-amplitude (K2) (secondary) | 159.7±11.7 km/s |
Details | |
Mass | 15.5±0.8[7] M☉ |
Luminosity (bolometric) | 59,279[8] L☉ |
Temperature | 24,200[8] K |
Rotational velocity (v sin i) | 315[9] km/s |
Age | 11.1±0.5[7] Myr |
Other designations | |
Database references | |
SIMBAD | data |
This is a suspected close spectroscopic binary system. The spectrum varies with a periodicity of 28.9 days, and a helium emission component shows a radial velocity variation that matches the period. The properties indicate it may be a φ Per-like system with a Be star primary and a hot subdwarf companion of type sdO. If this is the case, then the pair have a circular orbit with a period that matches the variability. The close-orbiting pair may have undergone interaction in the past, leaving the subdwarf stripped down and the primary star spinning rapidly.[6]
ο Puppis is slightly variable. The General Catalogue of Variable Stars lists it as a possible Be star with a magnitude range of 4.43 - 4.46.[11] The International Variable Star Index classifies it as a Lambda Eridani variable.[12]