Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Centaurus |
Right ascension | 13h 55m 32.38565s [1] |
Declination | −47° 17′ 18.1482″ [1] |
Apparent magnitude (V) | +2.55 [2] |
Characteristics | |
Spectral type | B2.5 IV [3] |
U−B color index | −0.91 [2] |
B−V color index | −0.22 [2] |
Astrometry | |
Radial velocity (Rv) | +6.5 [4] km/s |
Proper motion (μ) |
RA: −57.37
[1]
mas/
yr Dec.: −44.55 [1] mas/ yr |
Parallax (π) | 8.54 ± 0.13 mas [1] |
Distance | 382 ± 6
ly (117 ± 2 pc) |
Absolute magnitude (MV) | −2.79 [5] |
Orbit [6] | |
Period (P) | 8.024 days |
Semi-major axis (a) | 0.0014 " [7] |
Eccentricity (e) | 0.5 |
Periastron epoch (T) | 2413719.321 JD |
Argument of periastron (ω) (secondary) | 290° |
Details | |
Mass | 7.8±0.1 [3] M☉ |
Radius | 5.80±0.53 [8] R☉ |
Surface gravity (log g) | 3.84±0.08 [8] cgs |
Temperature | 23561±283 [8] K |
Rotational velocity (v sin i) | 235 [9] km/s |
Age | 39.8±5.7 [3] Myr |
Other designations | |
Database references | |
SIMBAD | data |
Zeta Centauri, Latinized from ζ Centauri, is a binary star system in the southern constellation of Centaurus. It has the proper name Alnair /æˈnɛər/, from Arabic: نير بطن قنطورس, romanized: nayyir baṭan qanṭūris, lit. 'the bright (star) of the body of the centaur'. [11] [12] With a combined apparent visual magnitude of +2.55, [2] it is one of the brighter members of the constellation. This system is close enough to the Earth that its distance can be measured directly using the parallax technique. This yields a value of roughly 382 light-years (117 parsecs), with a 1.6% margin of error. [1] It is drifting further away with a radial velocity of +6.5 km/s. [4]
In Chinese, 庫樓 (Kù Lóu), meaning Arsenal, refers to an asterism consisting of ζ Centauri, η Centauri, θ Centauri, 2 Centauri, HD 117440, ξ1 Centauri, γ Centauri, τ Centauri, D Centauri and σ Centauri. [13] Consequently, the Chinese name for ζ Centauri itself is 庫樓一 (Kù Lóu yī, English: the First Star of Arsenal.) [14]
ζ Cen is a double-lined spectroscopic binary system, [15] which indicates that the orbital motion was detected by shifts in the absorption lines of their combined spectra caused by the Doppler effect. The two stars orbit each other over a period of slightly more than eight days with an orbital eccentricity of about 0.5. [6] The estimated angular separation of the pair is 1.4 mas. [7]
At an estimated age of 40 million years, [3] the primary component of this system appears to be in the subgiant stage of its evolution with a stellar classification of B2.5 IV. [3] It is a large star with nearly 8 [3] times the mass of the Sun and close to 6 [8] times the Sun's radius. This star is rotating rapidly with a projected rotational velocity of 235 km s−1. [9]