Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Centaurus |
Right ascension | 12h 08m 05.22401s [2] |
Declination | −50° 39′ 40.5728″ [2] |
Apparent magnitude (V) | 4.47 [3] |
Characteristics | |
Spectral type | B6III [4] |
U−B color index | −0.67 [3] |
B−V color index | −0.15 [3] |
Variable type | rotating variable [5] |
Astrometry | |
Radial velocity (Rv) | 16.5 [3] km/s |
Proper motion (μ) |
RA: −35.16
[2]
mas/
yr Dec.: −6.47 [2] mas/ yr |
Parallax (π) | 7.44 ± 0.61 mas [2] |
Distance | 440 ± 40
ly (130 ± 10 pc) |
Absolute magnitude (MV) | −1.2±0.3 [4] |
Absolute bolometric magnitude (Mbol) | −2.9 ± 0.4 [4] |
Details | |
Mass | 5.7 ± 0.4 [5] M☉ |
Radius | 3.0 ± 0.6 [5] R☉ |
Luminosity | 1000+590 −370 [4] L☉ |
Surface gravity (log g) | 4.18 ± 0.15 [5] cgs |
Temperature | 17400 ± 400 [5] K |
Rotation | 1.295 ± 0.001 [5] days |
Rotational velocity (v sin i) | 90 [4] km/s |
Other designations | |
Database references | |
SIMBAD | data |
HD 105382 (also known as V863 Centauri) is a star in the constellation Centaurus. Its apparent magnitude is 4.47. From parallax measurements, it is located 130 parsecs (440 light years) from the Sun.
HD 105382 is a variable star whose apparent magnitude varies with an amplitude of 0.012 over a period of 1.295 days. It has been previously classified as a Be star, which would explain the variability as stellar pulsations, but this classification was probably due to accidental observation of the nearby Be star δ Centauri. [6] A 2004 study showed that the 1.295 day period is actually the rotation period of the star, and that the variability is caused by non-homogeneous distribution of elements in the stellar surface. In particular, HD 105382 is a helium-weak chemically peculiar star with a helium abundance varying between 0.5% and 15% of the solar abundance, and a silicon abundance varying between 0.00044% and 0.0069% the solar value. Regions with more helium appear to coincide with the regions with less silicon, and vice versa. [5] This peculiar abundance pattern is probably related to HD 105382's magnetic field, [5] which has a polar strength of 2.3 kG. [4]
From astrometric measurements by the Hipparcos spacecraft, HD 105382 is identified as a probable astrometric binary. [7] It is only 267" away from δ Centauri, and both stars appear to be at the same distance from Earth and have the same motion through space, so they may be related. In total, this may be a five star system. [8] It is a member of the Lower Centaurus–Crux (LCC) subgroup of the Scorpius–Centaurus association. [9]