14 Eridani

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14 Eridani
Observation data
Epoch J2000      Equinox
Constellation Eridanus
Right ascension 03h 16m 35.76908s[1]
Declination −09° 09′ 16.8515″[1]
Apparent magnitude (V) 6.143[2]
Spectral type F5 V Fe−0.7 CH−0.5[3]
B−V color index 0.399[2]
Radial velocity (Rv)−5.3±2.9[4] km/s
Proper motion (μ) RA: +6.97[1] mas/yr
Dec.: +351.73[1] mas/yr
Parallax (π)29.26 ± 0.72[1] mas
Distance111 ± 3 ly
(34.2 ± 0.8 pc)
Absolute magnitude (MV)3.47[5]
Mass1.31[6] M
Luminosity3.64[5] L
Surface gravity (log g)4.34±0.14[6] cgs
Temperature6,719±228[6] K
Metallicity [Fe/H]−0.10[7] dex
Age1.391[6] Gyr
Other designations
14 Eri, BD−09° 627, GC 3918, HD 20395, HIP 15244, HR 988, SAO 130395, PPM 185595, WDS J03158-0849B[8]
Database references

14 Eridani is a star in the Eridanus constellation. It has an apparent visual magnitude of 6.143[2] and is moving closer to the Sun with a radial velocity of around −5 km/s.[4] The measured annual parallax shift is 29.26 mas, which provides an estimated distance of about 111 light years. Proper motion studies indicate that this is an astrometric binary.[9][10] The visible component has a stellar classification of F5 V Fe−0.7 CH−0.5,[3] which indicates it has the spectrum of an F-type main-sequence star with underabundances of iron and methylidyne. The system has been detected as a source of X-ray emission.[11]


  1. ^ a b c d e van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752Freely accessible, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. 
  2. ^ a b c Høg, E.; et al. (2000), "The Tycho-2 catalogue of the 2.5 million brightest stars", Astronomy and Astrophysics, 355: L27, Bibcode:2000A&A...355L..27H, doi:10.1888/0333750888/2862. 
  3. ^ a b Gray, R. O.; et al. (2006), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc--The Southern Sample", The Astronomical Journal, 132: 161, arXiv:astro-ph/0603770Freely accessible, Bibcode:2006AJ....132..161G, doi:10.1086/504637. 
  4. ^ a b de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048Freely accessible, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, A61. 
  5. ^ a b Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971Freely accessible, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015. 
  6. ^ a b c d David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154Freely accessible, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146. 
  7. ^ Casagrande, L.; et al. (June 2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy and Astrophysics, 530: A138, arXiv:1103.4651Freely accessible, Bibcode:2011A&A...530A.138C, doi:10.1051/0004-6361/201016276. 
  8. ^ "14 Eri". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-01-27. 
  9. ^ Makarov, V. V.; Kaplan, G. H. (May 2005), "Statistical Constraints for Astrometric Binaries with Nonlinear Motion", The Astronomical Journal, 129 (5): 2420–2427, Bibcode:2005AJ....129.2420M, doi:10.1086/429590. 
  10. ^ Frankowski, A.; et al. (March 2007), "Proper-motion binaries in the Hipparcos catalogue. Comparison with radial velocity data", Astronomy and Astrophysics, 464 (1): 377–392, arXiv:astro-ph/0612449Freely accessible, Bibcode:2007A&A...464..377F, doi:10.1051/0004-6361:20065526. 
  11. ^ Huensch, M.; et al. (October 1998), "The ROSAT all-sky survey catalogue of optically bright main-sequence stars and subgiant stars", Astronomy and Astrophysics Supplement, 132: 155−171, Bibcode:1998A&AS..132..155H, doi:10.1051/aas:1998287.