107_Piscium

107 Piscium

107 Piscium

Star in the constellation Pisces

107 Piscium is a single[13] 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.[14] 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 24.8 light years 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.[15]

Quick Facts Constellation, Right ascension ...

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.[11] The star has 86% of the mass and 82% of the radius of the Sun,[9] but shines with only 46% of the Sun's luminosity.[8] The effective temperature of the star is 5,172 K.[9] It is rotating slowly with a period of 35.0 d.[10] The abundance of elements other than hydrogen and helium—the star's metallicity—is slightly lower than that of the Sun.[16] The level of chromospheric activity is similar to the Sun, and it shows a simple cycle of variation.[17][18]

107 Piscium has been examined for the presence of an infrared excess caused by exozodiacal dust, but none was detected.[19] 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.[19]

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.[20]

See also

References

  1. [1]
    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. [2]
    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. [3]
    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. [4]
    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. [5]
    "107 Psc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved September 24, 2008.
  6. [6]
    Lockwood, G. W.; et al. (August 1997). "The Photometric Variability of Sun-like Stars: Observations and Results, 1984-1995". The Astrophysical Journal. 485 (2): 789–811. Bibcode:1997ApJ...485..789L. doi:10.1086/304453.
  7. [7]
    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. S2CID 52952408.
  8. [8]
    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. [9]
    Fuhrmann, Klaus (2011). "Nearby stars of the Galactic disc and halo - V". Monthly Notices of the Royal Astronomical Society. 414 (4): 2893–2922. Bibcode:2011MNRAS.414.2893F. doi:10.1111/j.1365-2966.2011.18476.x.
  10. [10]
    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, S2CID 119209183.
  11. [11]
    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, S2CID 27151456.
  12. [12]
    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.
  13. [13]
    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.
  14. [14]
    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, S2CID 118445625
  15. [15]
    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. S2CID 56269929.
  16. [16]
    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.
  17. [17]
    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.
  18. [18]
    Wright, J. T.; et al. (August 2008). "The Jupiter Twin HD 154345b". The Astrophysical Journal Letters. 683 (1): L63–L66. arXiv:0802.1731. Bibcode:2008ApJ...683L..63W. doi:10.1086/587461. S2CID 16808434.
  19. [19]
    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, S2CID 16945896.
  20. [20]
    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, S2CID 55771565
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