107 Piscium
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107 Piscium
107 Piscium
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Pisces
Declination +20° 16′ 06.6602″[1]
5.14 to 5.26[2]
Spectral type K1V[3]
U-B color index +0.49[4]
B-V color index +0.84[4]
V-R color index 0.5[5]
R-I color index +0.43[4]
Variable type Constant[6]
Radial velocity (Rv)[7] km/s
Proper motion (?) RA: -301.592[1] mas/yr
Dec.: -674.505[1] mas/yr
Parallax (?)131.4903 ± 0.1515[1] mas
Distance24.80 ± 0.03 ly
(7.605 ± 0.009 pc)
Absolute magnitude (MV)5.87[8]
Mass[9] M
Radius[10] R
Luminosity (bolometric)0.46[8] L
Surface gravity (log g)4.50[8] cgs
Temperature[11] K
Metallicity [Fe/H]-0.04[9] dex
Rotation35.0 days[12]
Rotational velocity (v sin i)1[9] km/s
Age6.3[13] Gyr
Other designations
107 Psc, , GC 2080, HD 10476, HIP 7981, HR 493, SAO 74883, PPM 91014, , , LFT 153, LHS 1287, LTT 10596, NLTT 5685[5][14]
Database references

107 Piscium is a single[15]star in the constellation of Pisces. 107 Piscium is the star's Flamsteed designation. 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.[16] This star is faintly visible to the naked eye with an apparent visual magnitude that has been measured varying between 5.14 and 5.26.[2] However, that finding of variation was not confirmed by subsequent observations and is most likely spurious data.[6] It is located at a distance of about away from the Sun.[1] 107 Piscium is drifting closer to the Sun with a radial velocity of -33.6,[7] and is predicted to come as close as 15.4 light-years in around 135,800 years.[17]

This object is a K-type main-sequence star with a stellar classification of K1V,[3] indicating it is generating energy from core hydrogen fusion. It is somewhat older than the Sun--approximately 6 billion years old.[13] The star has 83%[9] of the mass and 80%[10] of the radius of the Sun, but shines with only 46% of the Sun's luminosity.[8] The effective temperature of the star is .[11] It is rotating slowly with a period of .[12] The abundance of elements other than hydrogen and helium--the star's metallicity--is slightly lower than that of the Sun.[9] The level of chromospheric activity is similar to the Sun, and it shows a simple cycle of variation.[18][19]

107 Piscium has been examined for the presence of an infrared excess caused by exozodiacal dust, but none was detected.[20] 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- (AU), where is the average distance from the Earth to the Sun.[20]

In 1997, based on data collected during the Hipparcos mission, the star was categorized as an astrometric binary with a period of . However, this result has not been not confirmed.[21]

See also


  1. ^ a b c d e f Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051.Gaia DR2 record for this source at VizieR.
  2. ^ a b 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 Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". The Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  4. ^ 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.
  5. ^ a b "107 Psc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2008.
  6. ^ a b Lockwood, G. W.; et al. (August 1997). "The Photometric Variability of Sun-like Stars: Observations and Results, 1984-1995". The Astrophysical Journal. 485 (2). Bibcode:1997ApJ...485..789L. doi:10.1086/304453.
  7. ^ a b Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv:1804.09370. Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795.
  8. ^ 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, Bibcode:2007PASJ...59..335T.
  9. ^ 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.
  10. ^ 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.
  11. ^ 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.
  12. ^ 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.
  13. ^ 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.
  14. ^ 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.
  15. ^ Halbwachs, J. -L; et al. (2018). "Multiplicity among solar-type stars. IV. The CORAVEL radial velocities and the spectroscopic orbits of nearby K dwarfs". Astronomy and Astrophysics. 619: A81. arXiv:1808.04605. Bibcode:2018A&A...619A..81H. doi:10.1051/0004-6361/201833377. S2CID 119437322.
  16. ^ 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
  17. ^ Bailer-Jones, C.A.L.; et al. (2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics. 616: A37. arXiv:1805.07581. Bibcode:2018A&A...616A..37B. doi:10.1051/0004-6361/201833456.
  18. ^ Radick, Richard R.; et al. (March 2018). "Patterns of Variation for the Sun and Sun-like Stars". The Astrophysical Journal. 855 (2): 28. Bibcode:2018ApJ...855...75R. doi:10.3847/1538-4357/aaaae3. 75.
  19. ^ Wright, J. T.; et al. (August 2008). "The Jupiter Twin HD 154345b". The Astrophysical Journal Letters. 683 (1). arXiv:0802.1731. Bibcode:2008ApJ...683L..63W. doi:10.1086/587461.
  20. ^ 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.
  21. ^ 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

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