HD 14214
  | |
| Observation data Epoch J2000[1] Equinox J2000[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−V color index | +0.588[6] |
| J−H color index | +0.484[1] |
| J−K color 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±0.0006 d |
| 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° |
| Periastron epoch (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 | |
| Database references | |
| SIMBAD | HD 14214 |
HD 14214 is a binary star in the constellation of Cetus. With an apparent magnitude of 5.60,[3] it can be faintly seen by the naked eye from Earth as a yellow-hued dot of light. As such, it is listed in the Bright Star Catalogue as HR 672. It is located at a distance of approximately 73.1 light-years (22.4 parsecs) according to Gaia DR3 parallax measurements.
Properties
[edit]This star system can be described as a single-lined (SB1) spectroscopic binary, a visual binary, and an interferometric binary.[5] This is unusual in that weak-lined field dwarfs have a small chance (5-15 %) of being in binary systems[11] (though HD 14214 A is now considered to be a subgiant 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 has fused all the hydrogen in its core into helium and evolved past the main sequence, with the spectral type G0IV or G0.5IVb (the "b" suffix in the latter indicates that it is slightly less luminous than a typical G0.5IV subgiant[12]). It is slightly hotter and more massive than the Sun, but 64% larger and 2.76 times as luminous. It has an age of about 4.5 billion years, similar to the age of the Solar System.
The secondary star, whose spectra cannot be directly observed, is likely a red dwarf, with the spectral type M0V, a little over half the mass of the Sun, and 40% the radius, but only radiates 4% the luminosity from its photosphere.
Nearby objects
[edit]It appears very close in the sky to PKS 0215+015, a BL Lacertae object with a resting apparent magnitude of 18.3 in the V band. Anti-blooming techniques have been devised in order to counter severe blooming caused by the far brighter HD 14214 during photometric observations of the object.[13]
See also
[edit]References
[edit]- ^ a b c d "HD 14214". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 22 November 2024.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e f g Fekel, Francis C.; Williamson, Michael; Pourbaix, D. (2007). "The Spectroscopic and Astrometric Orbits of HR 672". The Astronomical Journal. 133 (6): 2431–2434. doi:10.1086/516574. ISSN 0004-6256.
- ^ Osten, R. A.; Saar, S. H. (1 April 1998). "Physical properties of active stars and stellar systems". Monthly Notices of the Royal Astronomical Society. 295 (2): 257–264. doi:10.1046/j.1365-8711.1998.01121.x. ISSN 0035-8711.
- ^ a b Abt, Helmut A.; Willmarth, Daryl (2006). "The Secondaries of Solar-Type Primaries. I. The Radial Velocities". The Astrophysical Journal Supplement Series. 162 (1): 207–226. doi:10.1086/498095. ISSN 0067-0049.
Note: This source erroneously assigns the Bayer designation λ2 Fornacis to the star, which actually belongs to HD 16417 (HR 772). - ^ a b c d Wang, Xiaoli; Ren, Shulin; Fu, Yanning (14 September 2015). "Self-Consistent Orbits and Physical Properties for Eight Single-Lined Spectroscopic Binaries". The Astronomical Journal. 150 (4): 110. doi:10.1088/0004-6256/150/4/110. ISSN 1538-3881.
- ^ Pourbaix, D.; Tokovinin, A. A.; Batten, A. H.; Fekel, F. C.; Hartkopf, W. I.; Levato, H.; Morrell, N. I.; Torres, G.; Udry, S. (2004). "SB9 The ninth catalogue of spectroscopic binary orbits". Astronomy & Astrophysics. 424 (2): 727–732. doi:10.1051/0004-6361:20041213. ISSN 0004-6361.
- ^ Malyuto, V.; Shvelidze, T. (1 January 2011). "Determination of Homogenized Effective Temperatures from Stellar Catalogs". Open Astronomy. 20 (1). doi:10.1515/astro-2017-0271. ISSN 2543-6376.
- ^ Barry, D. C.; Cromwell, R. H.; Hege, K.; Schoolman, S. A. (1981). "Chromospheric decay and the ages of solar type stars". The Astrophysical Journal. 247: 210. doi:10.1086/159027. ISSN 0004-637X.
- ^ Pilcher, Frederick. "Uranometria Argentina". Archived from the original on 27 February 2012. Retrieved 1 November 2024.
- ^ Willmarth, D.; Abt, H. A. (March 1986). "The Binary Frequency Among Weak-Lined Dwarfs". Bulletin of the American Astronomical Society. 18: 681. Bibcode:1986BAAS...18..681W.
- ^ D.S. Hayes; L.E. Pasinetti; A.G. Davis Philip (6 December 2012). Calibration of Fundamental Stellar Quantities: Proceedings of the 111th Symposium of the International Astronomical Union held at Villa Olmo, Como, Italy, May 24–29, 1984. Springer Science & Business Media. pp. 129–. ISBN 978-94-009-5456-4.
- ^ Neely, A. William; Janesick, James R. (1993). "A CCD antiblooming technique for use in photometry". Publications of the Astronomical Society of the Pacific. 105: 1330. doi:10.1086/133314. ISSN 0004-6280.
