HD 90264
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| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Carina |
| Right ascension | Template:RA[1] |
| Declination | Template:DEC[1] |
| Apparent magnitude (V) | 4.97[2] |
| Characteristics | |
| Spectral type | B8V[3] |
| B−V Template:Engvar | Script error: No such module "val".[2] |
| Astrometry | |
| Radial velocity (Rv) | Script error: No such module "val".[2] km/s |
| Proper motion (μ) | RA: −22.39[1] mas/yr Dec.: +11.48[1] mas/yr |
| Parallax (π) | 8.12±0.18 mas[1] |
| Distance | Template:Rnd ± Template:Rnd ly (Template:Rnd ± Template:Rnd pc) |
| Absolute magnitude (MV) | −0.403[4] |
| Orbit[4] | |
| Period (P) | Script error: No such module "val". |
| Semi-major axis (a) | Script error: No such module "val". |
| Eccentricity (e) | Script error: No such module "val". |
| Inclination (i) | 54° |
| Periastron epoch (T) | Script error: No such module "val". |
| Argument of periastron (ω) (secondary) | Script error: No such module "val".° |
| Semi-amplitude (K1) (primary) | Script error: No such module "val". km/s |
| Semi-amplitude (K2) (secondary) | Script error: No such module "val". km/s |
| Details | |
| A | |
| Mass | 4.3[4] Template:Solar mass |
| Luminosity | 288.39[2] Template:Solar luminosity |
| Rotational velocity (v sin i) | 7[4] km/s |
| Age | 18[4] Myr |
| B | |
| Mass | 3.5[4] Template:Solar mass |
| Metallicity [Fe/H] | {{{metal_fe2}}} dex |
| Other designations | |
| Template:Odlist[5] | |
| Database references | |
| SIMBAD | data |
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HD 90264 is a binary star[4] 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.[2] 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.[2] The system is a member of the Lower Centaurus Crux association of the Sco-Cen Complex.[4]
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 Script error: No such module "convert".. 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.[4]
References
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