Chi Ceti

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Chi Ceti
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Cetus
HD 11171
Right ascension  01h 49m 35.10316s[1]
Declination −10° 41′ 11.0674″[1]
Apparent magnitude (V) 4.66[2]
HD 11131
Right ascension  01h 49m 23.35579s[1]
Declination −10° 42′ 12.8594″[1]
Apparent magnitude (V) 6.75[2]
HD 11171
Spectral type F3 III[3] or F0 V[4]
U−B color index +0.04[2]
B−V color index +0.33[2]
HD 11131
Spectral type G3 V[4]
U−B color index +0.12[2]
B−V color index +0.61[2]
Variable type BY Dra[5]
HD 11171
Radial velocity (Rv)−1.8[3] km/s
Proper motion (μ) RA: −148.11[1] mas/yr
Dec.: −93.43[1] mas/yr
Parallax (π)43.13 ± 0.26[1] mas
Distance75.6 ± 0.5 ly
(23.2 ± 0.1 pc)
Absolute magnitude (MV)+2.83±0.01[6]
HD 11131
Radial velocity (Rv)−3.89±0.12[7] km/s
Proper motion (μ) RA: −124.54[1] mas/yr
Dec.: −105.82[1] mas/yr
Parallax (π)44.32 ± 3.02[1] mas
Distance74 ± 5 ly
(23 ± 2 pc)
Absolute magnitude (MV)4.98[8]
HD 11171
Mass1.36[3] M
Luminosity5.6[3] L
Temperature6,746±258[3] K
Metallicity [Fe/H]0.14[6] dex
Age1.2[3] Gyr
HD 11131
Surface gravity (log g)4.53[9] cgs
Temperature5,804[9] K
Metallicity [Fe/H]−0.09[9] dex
Rotational velocity (v sin i)3.34[10] km/s
Other designations
χ Cet, Gj 9061, ENG 8
χ Ceti A: 53 Cet, HD 11171, BD−11° 352, FK5 1051, HIP 8497, HR 531, SAO 148036.[11]
χ Ceti B: EZ Cet, HD 11131, BD−11°351, HIP 8486, SAO 148033.[12]
Database references
χ Ceti A
χ Ceti B

Chi Ceti (χ Ceti), is the Bayer designation for a double star in the equatorial constellation of Cetus. They appear to be common proper motion companions, sharing a similar motion through space.[13] The brighter component, HD 11171, is visible to the naked eye with an apparent visual magnitude of 4.66, while the fainter companion, HD 11131, is magnitude 6.75.[2] Both lie at roughly the same distance, with the brighter component lying at an estimated distance of 75.6 light years from the Sun based upon an annual parallax shift of 43.13 mass.[1]

The primary, component A, is an evolved K-type giant star with a stellar classification of F3 III.[3] However, Houk and Swift (1999) listed a classification of F0 V,[4] which would match an F-type main sequence star. It displays an infrared excess at a wavelength of 70 μm and thus is a candidate host of an orbiting debris disk.[14]

The common proper motion companion, component B, is a G-type main sequence star with a classification of G3 V.[4] It is a BY Draconis variable with a periodicity of 8.92 days and a variable star designation of EZ Cet.[5]


  1. ^ a b c d e f g h i j k van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357.
  2. ^ a b c d e f g Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data: 0, Bibcode:1986EgUBV........0M.
  3. ^ a b c d e f g Luck, R. Earle (September 2015), "Abundances in the Local Region. I. G and K Giants", The Astronomical Journal, 150 (3): 23, arXiv:1507.01466, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, 88.
  4. ^ a b c d Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5: 0, Bibcode:1999MSS...C05....0H.
  5. ^ a b Kazarovets, E. V.; et al. (2006), "The 78th Name-List of Variable Stars", Information Bulletin on Variable Stars, 5721: 1, Bibcode:2006IBVS.5721....1K.
  6. ^ a b Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191.
  7. ^ 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:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, A61.
  8. ^ Porto de Mello, G. F.; et al. (March 2014), "A photometric and spectroscopic survey of solar twin stars within 50 parsecs of the Sun; I. Atmospheric parameters and color similarity to the Sun", Astronomy and Astrophysics, 563: A52, arXiv:1312.7571, Bibcode:2014A&A...563A..52P, doi:10.1051/0004-6361/201322277.
  9. ^ a b c Datson, Juliet; et al. (February 2015), "Spectroscopic study of solar twins and analogues", Astronomy & Astrophysics, 574: 12, arXiv:1412.8168, Bibcode:2015A&A...574A.124D, doi:10.1051/0004-6361/201425000, A124.
  10. ^ Martínez-Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter", Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725.
  11. ^ "chi Cet". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-02-12.
  12. ^ V* EZ Cet.
  13. ^ Soderblom, David R.; Mayor, Michel (January 1993), "Stellar kinematic groups. I - The Ursa Major group", Astronomical Journal, 105 (1): 226–249, Bibcode:1993AJ....105..226S, doi:10.1086/116422.
  14. ^ Koerner, D. W.; et al. (February 2010), "New Debris Disk Candidates Around 49 Nearby Stars" (PDF), The Astrophysical Journal Letters, 710 (1): L26–L29, Bibcode:2010ApJ...710L..26K, doi:10.1088/2041-8205/710/1/L26.

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