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Star in the constellation Centaurus From Wikipedia, the free encyclopedia
H Centauri (H Cen), also known as V945 Centauri, is probable triple star system[3] located in the constellation Centaurus. From parallax measurements, it is located 113 parsecs (370 light years) from the Sun. It is a member of the Lower Centaurus–Crux (LCC) subgroup of the Scorpius–Centaurus association.[4]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Centaurus |
Right ascension | 12h 57m 04.35244s[2] |
Declination | −51° 11′ 55.5058″[2] |
Apparent magnitude (V) | 5.163[2] |
Characteristics | |
Spectral type | B7V + B8.5V + B[3] |
Apparent magnitude (B) | 5.102 |
Apparent magnitude (V) | 5.163 |
Variable type | ellipsoidal variable[3] |
Astrometry | |
Radial velocity (Rv) | 14.55 ± 1.6[3] km/s |
Proper motion (μ) | RA: −30.15 mas/yr Dec.: −14.61 mas/yr |
Parallax (π) | 8.85 ± 0.27 mas |
Distance | 370 ± 10 ly (113 ± 3 pc) |
Details[3] | |
Primary | |
Mass | 3.32 ± 0.51 M☉ |
Radius | 2.09 ± 0.12 R☉ |
Luminosity | 111 ± 21 L☉ |
Surface gravity (log g) | 4.3 ± 0.1 cgs |
Temperature | 13000 K |
Secondary | |
Mass | 2.37 ± 0.48 M☉ |
Radius | 1.67 ± 0.09 R☉ |
Luminosity | 37 ± 7 L☉ |
Surface gravity (log g) | 4.4 ± 0.1 cgs |
Temperature | 10687 ± 52 K |
Other designations | |
Database references | |
SIMBAD | data |
This system is a double-lined spectroscopic binary formed by two B-type main-sequence star with spectral types B7V and B8.5V. They are in a close (but detached) circular orbit with a period of 0.6496 days and a separation of 5.63 solar radii. Observed at an inclination of 24°, the system is an ellipsoidal variable whose apparent visual magnitude varies from 5.14 to 5.17 over the course of an orbit as the star's visible surface area changes. The system's spectrum contains a third set of spectral lines that are probably from a third star, also of type B.[3]
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