Observation data Epoch J2000.0 Equinox J2000.0 | |
---|---|
Constellation | Centaurus |
Right ascension | 13h 51m 49.60s[1] |
Declination | −32° 59′ 38.7″[1] |
Apparent magnitude (V) | 4.32[2] (4.52 + 5.97)[3] |
Characteristics | |
Spectral type | B5 III-IVp[4] + B8 V[5] |
B−V color index | −0.146±0.003[2] |
Variable type | Eclipsing?[6] |
Astrometry | |
Radial velocity (Rv) | +7.5±1.6[7] km/s |
Absolute magnitude (MV) | −0.46[2] |
A | |
Proper motion (μ) | RA: −34.698±0.864[8] mas/yr Dec.: −27.909±0.792[8] mas/yr |
Parallax (π) | 11.0982 ± 0.4267 mas |
Distance | 290 ± 10 ly (90 ± 3 pc) |
B | |
Proper motion (μ) | RA: −36.737±0.266[9] mas/yr Dec.: −23.774±0.189[9] mas/yr |
Parallax (π) | 10.2659 ± 0.1380 mas[9] |
Distance | 318 ± 4 ly (97 ± 1 pc) |
Orbit[10] | |
Primary | Ba |
Companion | Bb |
Period (P) | 17.428 d |
Eccentricity (e) | 0.21 |
Periastron epoch (T) | 2443296.44 JD |
Argument of periastron (ω) (secondary) | 15° |
Semi-amplitude (K1) (primary) | 17 km/s |
Details | |
3 Cen A | |
Mass | 5.0±0.1[11] M☉ |
Surface gravity (log g) | 3.80[12] cgs |
Temperature | 17,500[12] K |
Age | 47.4±7.3[11] Myr |
3 Cen B | |
Mass | 2.47±0.10[5] M☉ |
Radius | 2.8[13] R☉ |
Luminosity | 50.2+11.7 −9.5[5] L☉ |
Temperature | 9,638+67 −66[5] K |
Rotational velocity (v sin i) | 135[5] km/s |
Other designations | |
3 Cen A: GC 18724, HD 120709, HR 5210, SAO 204916 | |
3 Cen B: GC 18725, HD 120710, HR 5211, SAO 204917 | |
Database references | |
SIMBAD | data |
A | |
B |
3 Centauri is a triple star[3] system in the southern constellation of Centaurus,[14] located approximately 300 light years from the Sun.[8][9] It is visible to the naked eye as a faint, blue-white hued star with a combined apparent visual magnitude of 4.32.[2] As of 2017, the two visible components had an angular separation of 7.851″ along a position angle of 106°.[3] The system has the Bayer designation k Centauri; 3 Centauri is the Flamsteed designation. It was a suspected eclipsing binary with a variable star designation V983 Centauri,[6] however the AAVSO website lists it as non-variable, formerly suspected to be variable.[15]
The brighter member, designated component A, is a magnitude 4.52[3] chemically peculiar star of the helium-weak (CP4) variety, and has a stellar classification of B5 III-IVp.[4] The spectrum of the star displays overabundances of elements such as nitrogen, phosphorus, manganese, iron, and nickel, while carbon, oxygen, magnesium, aluminium, sulfur, and chlorine appear underabundant relative to the Sun.[12] Weak emission line features are also visible.[16]
The magnitude 5.97[3] secondary, component B, is a single-lined spectroscopic binary star system with an orbital period of 17.4 days and an eccentricity of 0.21.[10] The pair have an angular separation of 2.485 mas. The visible component is a B-type main-sequence star with a class of B8 V.[5]
van Leeuwen2007
was invoked but never defined (see the help page).Anderson2012
was invoked but never defined (see the help page).Veramendi2014
was invoked but never defined (see the help page).Sigut2000
was invoked but never defined (see the help page).zorec2012
was invoked but never defined (see the help page).Samus2017
was invoked but never defined (see the help page).Gontcharov2006
was invoked but never defined (see the help page).dr2a
was invoked but never defined (see the help page).dr2b
was invoked but never defined (see the help page).Pourbaix2004
was invoked but never defined (see the help page).Tetzlaff2011
was invoked but never defined (see the help page).Sadakane2018
was invoked but never defined (see the help page).PasinettiFracassini2001
was invoked but never defined (see the help page).SIMBAD
was invoked but never defined (see the help page).AAVSO
was invoked but never defined (see the help page).Wahlgren2004
was invoked but never defined (see the help page).