HD 90264
HD 90264 is a binary star system in the southern constellation of Carina. It has the Bayer designation of L Carinae, while HD 90264 is the star's identifier in the Henry Draper catalogue. This system has a blue-white hue and is faintly visible to the naked eye with an apparent visual magnitude of 4.97. It is located at a distance of approximately 402 light years from the Sun based on parallax, and is drifting further away with a radial velocity of around +12 km/s. The system is a member of the Lower Centaurus Crux association of the Sco-Cen Complex.
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Carina |
| Right ascension | 10h 22m 58.14606s |
| Declination | −66° 54′ 05.3903″ |
| Apparent magnitude (V) | 4.97 |
| Characteristics | |
| Spectral type | B8V |
| B−V color index | −0.128±0.003 |
| Astrometry | |
| Radial velocity (Rv) | +12.0±4.2 km/s |
| Proper motion (μ) | RA: −22.39 mas/yr Dec.: +11.48 mas/yr |
| Parallax (π) | 8.12 ± 0.18 mas |
| Distance | 402 ± 9 ly (123 ± 3 pc) |
| Absolute magnitude (MV) | −0.403 |
| Orbit | |
| Period (P) | 15.727±0.001 d |
| Semi-major axis (a) | 52.66 R☉ |
| Eccentricity (e) | 0.044±0.014 |
| Inclination (i) | 54° |
| Periastron epoch (T) | 2,452,814.78±1.05 JD |
| Argument of periastron (ω) (secondary) | 138±25° |
| Semi-amplitude (K1) (primary) | 62.2±1.9 km/s |
| Semi-amplitude (K2) (secondary) | 76.0±1.5 km/s |
| Details | |
| A | |
| Mass | 4.3 M☉ |
| Luminosity | 288.39 L☉ |
| Rotational velocity (v sin i) | 7 km/s |
| Age | 18 Myr |
| B | |
| Mass | 3.5 M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
This system was found to be a close double-lined spectroscopic binary in 1977, consisting of two B-type main-sequence stars. It has a near circular orbit with a period of 15.727 days and a semimajor axis of 0.2449 AU. They appear to be spin-orbit synchronized. Both stars appear to be deficient in helium. The primary is a helium variable star while the companion is a mercury-manganese star. The variability of both stars aligns favorably with the orbital period.