107 Piscium

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107 Piscium
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Pisces
Right ascension 01h 42m 29.7619s[1]
Declination +20° 16′ 06.616″[1]
Apparent magnitude (V) 5.14 to 5.26[2]
Spectral type K1V[1]
U−B color index +0.49[3]
B−V color index +0.84[3]
V−R color index 0.5[1]
R−I color index +0.43[3]
Variable type Suspected[2]
Radial velocity (Rv)−33.5 ± 0.9[1] km/s
Proper motion (μ) RA: −302.14[1] mas/yr
Dec.: −677.46[1] mas/yr
Parallax (π)133.92 ± 0.91[1] mas
Distance24.4 ± 0.2 ly
(7.47 ± 0.05 pc)
Absolute magnitude (MV)5.87[4]
Mass0.83 (0.80 to 0.89)[5] M
Radius0.80 ± 0.06[6] R
Luminosity (bolometric)0.46[4] L
Surface gravity (log g)4.50[4] cgs
Temperature5242 ± 3.2[7] K
Metallicity [Fe/H]−0.04[5] dex
Rotation35.0 days[8]
Rotational velocity (v sin i)1[5] km/s
Age6.3[9] Gyr
Other designations
BD+19° 279, CCDM J01425+2016A, GC 2080, Gliese 68, HD 10476, HIP 7981, HR 493, IDS 01371+1947 A, LFT 153, LHS 1287, LTT 10596, NLTT 5685, PPM 91014, SAO 74883, WDS 01425+2016A.[1][10]
Database references

107 Piscium (abbreviated 107 Psc) is a K-type main sequence star in the constellation of Pisces, about 24.4 light years away from the Earth.[1] 107 Piscium is the Flamsteed designation. It has an apparent visual magnitude which varies between 5.14 and 5.26.[2]


John Flamsteed numbered the stars of Pisces from 1 to 113, publishing his Catalogus Britannicus in 1725. He accidentally numbered 107 Piscium twice, as he also allocated it the designation of 2 Arietis.[11]


The star is somewhat older than the Sun—approximately 6 billion years old.[9] It has 83%[5] of the mass and 80%[6] of the radius of the Sun, but shines with only 46% of the Sun's luminosity.[4] The effective temperature of the star is 5,242 K.[7] It is rotating slowly with a period of 35.0 days.[8] The abundance of elements other than hydrogen and helium—the star's metallicity—is slightly lower than that of the Sun.[5]

107 Piscium has been examined for the presence of an infrared excess caused by exozodiacal dust, but none was detected.[12] The habitable zone for this star, defined as the locations where liquid water could be present on an Earth-like planet, is at a radius of 0.52–1.10 Astronomical Units (AU), where 1 AU is the average distance from the Earth to the Sun.[12]

In 1997, based on data collected during the Hipparcos mission, the star was categorized as an astrometric binary with a period of 0.576 years. However, this result has not been not confirmed.[13]

See also[edit]


  1. ^ a b c d e f g h i j "107 Psc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved September 24, 2008.
  2. ^ a b c NSV 600, database entry, New Catalogue of Suspected Variable Stars, the improved version, Sternberg Astronomical Institute, Moscow, Russia. Accessed on line September 24, 2008.
  3. ^ a b c HR 493, database entry, The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version), D. Hoffleit and W. H. Warren, Jr., CDS ID V/50. Accessed on line September 24, 2008.
  4. ^ a b c d HD 10476, catalog entry, Fundamental parameters and elemental abundances of 160 F-G-K stars based on OAO spectrum database, Y. Takeda, CDS ID J/PASJ/59/335; see also Publications of the Astronomical Society of Japan 59, #2 (April 2007), pp. 335–356, Bibcode2007PASJ...59..335T.
  5. ^ a b c d e HD 10476, database entry, The Geneva-Copenhagen Survey of Solar neighbourhood, J. Holmberg et al., 2007, CDS ID V/117A. Accessed on line November 19, 2008.
  6. ^ a b Perrin, M.-N. (1987), "Stellar radius determination from IRAS 12-micron fluxes", Astronomy and Astrophysics, 172: 235–240, Bibcode:1987A&A...172..235P.
  7. ^ a b Kovtyukh; Soubiran, C.; Belik, S. I.; Gorlova, N. I. (2003), "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios", Astronomy and Astrophysics, 411 (3): 559–564, arXiv:astro-ph/0308429, Bibcode:2003A&A...411..559K, doi:10.1051/0004-6361:20031378.
  8. ^ a b Maldonado, J.; et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics, 521: A12, arXiv:1007.1132, Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948.
  9. ^ a b Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal, 687 (2): 1264–1293, arXiv:0807.1686, Bibcode:2008ApJ...687.1264M, doi:10.1086/591785.
  10. ^ Entry 01425+2016, The Washington Double Star Catalog Archived 2008-04-12 at the Wayback Machine., United States Naval Observatory. Accessed on line September 24, 2008.
  11. ^ Wagman, M. (August 1987), "Flamsteed's Missing Stars", Journal for the History of Astronomy, 18 (3): 213, Bibcode:1987JHA....18..209W, doi:10.1177/002182868701800305
  12. ^ a b Absil, O.; et al. (July 2013), "A near-infrared interferometric survey of debris-disc stars. III. First statistics based on 42 stars observed with CHARA/FLUOR", Astronomy and Astrophysics, 555: A104, arXiv:1307.2488, Bibcode:2013A&A...555A.104A, doi:10.1051/0004-6361/201321673.
  13. ^ Agati, J.-L.; et al. (February 2015), "Are the orbital poles of binary stars in the solar neighbourhood anisotropically distributed?", Astronomy and Astrophysics, 574: A6, arXiv:1411.4919, Bibcode:2015A&A...574A...6A, doi:10.1051/0004-6361/201323056

External links[edit]