  | |
| Observation data EpochJ2000[1] EquinoxJ2000[1] | |
|---|---|
| Constellation | Cetus |
| Right ascension | 02h 18m 01.44332s[2] |
| Declination | +01° 45′ 28.1235″[2] |
| Apparent magnitude (V) | 5.60[3] |
| Characteristics | |
| Spectral type | G0IV[4] or G0.5IVb[5] (A) ~M0V[3] (B) |
| B−Vcolor index | +0.588[6] |
| J−Hcolor index | +0.484[1] |
| J−Kcolor index | +0.569[1] |
| Astrometry | |
| Radial velocity (Rv) | 25.72±0.01[7] km/s |
| Proper motion (μ) | RA: 366.090[2]mas/yr Dec.: 369.815[2]mas/yr |
| Parallax (π) | 44.5963±0.3470 mas[2] |
| Distance | 73.1 ± 0.6 ly (22.4 ± 0.2 pc) |
| Absolute magnitude (MV) | 3.69 (combined)[6] |
| Orbit[6] | |
| Primary | HD 14214 A |
| Companion | HD 14214 B |
| Period (P) | 93.2874±0.0006d |
| Semi-major axis (a) | (21.05±0.01)×106 km (minimum)[3] |
| Eccentricity (e) | 0.5217±0.0002 |
| Inclination (i) | 105.1±3.5° |
| Longitude of the node (Ω) | 281.0±3.1° |
| Periastronepoch (T) | 54094.633±0.005 |
| Argument of periastron (ω) (secondary) | 103.87±0.03° |
| Details[6] | |
| HD 14214 A | |
| Mass | 1.15,[3] 1.20 M☉ |
| Radius | 1.64±0.07[3] R☉ |
| Luminosity | 2.76 L☉ |
| Temperature | 6032±23[8] K |
| Metallicity[Fe/H] | 0.021±0.001 dex |
| Rotational velocity (v sin i) | 2.1±1[3] km/s |
| Age | 4.56,[9] 4.47 Gyr |
| HD 14214 B | |
| Mass | 0.53 M☉ |
| Radius | 0.4 R☉ |
| Luminosity | 0.04 L☉ |
| Other designations | |
| 232 G. Ceti,AG+01°242,BD+01°410,Gaia DR3 2513664248895784192,GC 2770,HD 14214,HIP 10723,HR 672,SAO 110456,PPM 145462,TIC 419994887,TYC 38-1343-1,2MASS J02180145+0145282,WISEA J021801.69+014531.9[1][10] | |
| Database references | |
| SIMBAD | HD 14214 |
HD 14214 is abinary star in theconstellation ofCetus. With anapparent magnitude of 5.60,[3] it can be faintly seen by thenaked eye fromEarth as a yellow-hued dot of light. As such, it is listed in theBright Star Catalogue asHR 672. It is located at a distance of approximately 73.1 light-years (22.4 parsecs) according toGaia DR3parallax measurements.
This star system can be described as a single-lined (SB1)spectroscopic binary, a visual binary, and aninterferometric binary.[5] This is unusual in that weak-linedfielddwarfs have a small chance (5-15 %) of being in binary systems[11] (though HD 14214 A is now considered to be asubgiant rather than a dwarf). The two stars orbit each other in a fairly elliptical (eccentricity 0.5217) orbit every 93.2874 days.
The primary star is a subgiant, a star that hasfused all thehydrogen in itscore intohelium andevolved past themain sequence, with thespectral type G0IV or G0.5IVb (the "b" suffix in the latter indicates that it is slightly lessluminous than a typical G0.5IV subgiant[12]). It is slightly hotter and more massive than theSun, but 64% larger and 2.76 times as luminous. It has an age of about 4.5 billion years, similar to theage of the Solar System.
The secondary star, whosespectra cannot be directly observed, is likely ared dwarf, with the spectral type M0V, a little over half themass of the Sun, and 40% theradius, but only radiates 4% theluminosity from itsphotosphere.
It appears very close in the sky toPKS 0215+015, aBL Lacertae object with a resting apparent magnitude of 18.3 in theV band.Anti-blooming techniques have been devised in order to counter severe blooming caused by the far brighter HD 14214 duringphotometric observations of the object.[13]
