Epsilon Ceti

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Epsilon Ceti
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Cetus
Right ascension 02h 39m 33.82853s[1]
Declination −11° 52′ 19.7132″[1]
Apparent magnitude (V) +4.84[2]
Spectral type F2V + F7/G4V[3]
U−B color index −0.02[2]
B−V color index +0.45[2]
Proper motion (μ) RA: +161.62[1] mas/yr
Dec.: −230.53[1] mas/yr
Parallax (π) 35.1 ± 1.0[1] mas
Distance 93 ± 3 ly
(28.5 ± 0.8 pc)
Period (P) 2.6512±0.0005 yr
Semi-major axis (a) 0.1063±0.0005
Eccentricity (e) 0.230±0.001
Inclination (i) 24.2±0.2°
Longitude of the node (Ω) 90.2±0.2°
Periastron epoch (T) 2012.3109±0.0005
Argument of periastron (ω)
ε Cet A
Mass 1.37±0.09[3] M
Surface gravity (log g) 4.21±0.14[4] cgs
Temperature 6,537±222[4] K
Age 1.8[4] Gyr
ε Cet B
Mass 1.03±0.08[3] M
Other designations
ε Cet, 83 Cet, BD−12° 501, HD 16620, HIP 12390, HR 781, SAO 148528.[5]
Database references

Epsilon Ceti (ε Ceti) is the Bayer designation for a binary star system located in the equatorial constellation of Cetus. It is faintly visible to the naked eye with an apparent visual magnitude of +4.84.[2] Based upon an annual parallax shift of 14.58 mas,[1] it is located around 98 light years away from the Sun.

This is a line-width spectroscopic binary star system. It has an orbital period of 2.65 years and an eccentricity of 0.23. The semimajor axis is 0.11 AU, or 11% of the distance between the Sun and the Earth, and the orbital plane is inclined at an angle of 24.2°.The primary member, component A, is an F-type main sequence star with a stellar classification of F2 V. The spectrum of the secondary, component B, can not be readily separated from that of the primary, so its type can only be estimated as a main sequence star lying in the range between F7 V and G4 V.[3] The system is estimated to be 1.8 billion years old,[4] with the primary having 1.4 times the mass of the Sun and the secondary being about equal to the Sun's mass.[3]


  1. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, Bibcode:2007A&A...474..653V, arXiv:0708.1752Freely accessible, doi:10.1051/0004-6361:20078357. 
  2. ^ a b c d Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV data, SIMBAD, Bibcode:1986EgUBV........0M. 
  3. ^ a b c d e f Docobo, J. A.; Andrade, M. (2013), "Dynamical and physical properties of 22 binaries discovered by W. S. Finsen", Monthly Notices of the Royal Astronomical Society, 428 (1): 321–339, Bibcode:2013MNRAS.428..321D, doi:10.1093/mnras/sts045. 
  4. ^ 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, Bibcode:2015ApJ...804..146D, arXiv:1501.03154Freely accessible, doi:10.1088/0004-637X/804/2/146. 
  5. ^ "eps Cet -- Spectroscopic binary", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-02-04.