Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Centaurus |
Right ascension | 14h 32m 33.0833s [2] |
Declination | −56° 53′ 15.774″ [2] |
Apparent magnitude (V) | 6.42 - 7.22 [3] |
Characteristics | |
Spectral type | F5 Ib/II [4] |
B−V color index | 0.87 [5] |
Variable type | Classical Cepheid [3] |
Astrometry | |
Radial velocity (Rv) | −18.90 ± 1.4 [6] km/s |
Proper motion (μ) | RA: −6.697 [2] mas/yr Dec.: −7.068 [2] mas/yr |
Parallax (π) | 1.3898±0.0221 mas [2] |
Distance | 2,350 ± 40 ly (720 ± 10 pc) |
Details | |
Mass | 4.3 [7] M☉ |
Radius | 40 [2] R☉ |
Luminosity | 1,657 [8] L☉ |
Surface gravity (log g) | 1.89 [2] cgs |
Temperature | 5,500 [8] K |
Metallicity [Fe/H] | +0.12 [9] dex |
Age | 103 [10] Myr |
Other designations | |
V Cen, CD−56°5479, HD 127297, HIP 71116, HR 5421, SAO 241777 [5] | |
Database references | |
SIMBAD | data |
V Centauri (V Cen) is a Classical Cepheid variable, a type of variable star, in the constellation Centaurus. It is approximately 2,350 light-years (720 parsecs) away based on parallax.
Alexander W. Roberts discovered this star in 1894, and from 267 visual observations he determined is period of variation. [11] V Centauri varies regularly between visual magnitudes 6.42 and 7.22 every 5.5 days. It is classified as a Cepheid variable on the basis of its light variations, with the brightness increase from minimum to maximum taking only a third of the time of the decrease from maximum to minimum. Cepheids are pulsating variable stars and V Centauri expands and contracts over its pulsation cycle as well as changing temperature. [3]
According to the South African Astronomical Observatory, the chemical composition was derived as being high in sodium (Na) and aluminium (Al) and low in magnesium (Mg). [12] Following a normal composition for a Cepheid star, V Cen does not have any unusual characteristics. V Centauri's composition was observed alongside six other Classical Cepheid variable stars with the support of Russian, Chilean, and Ukrainian observatories. [12]