Astronomy:107 Piscium

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Short description: Star in the constellation Pisces
107 Piscium
Observation data
Equinox J2000.0]] (ICRS)
Constellation Pisces
Right ascension  01h 42m 29.76349s[1]
Declination +20° 16′ 06.6602″[1]
Apparent magnitude (V) 5.14 to 5.26[2]
Characteristics
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]
Astrometry
Radial velocity (Rv)−33.619±0.0013[7] km/s
Proper motion (μ) RA: −301.592[1] mas/yr
Dec.: −674.505[1] mas/yr
Parallax (π)131.4903 ± 0.1515[1] mas
Distance24.80 ± 0.03 ly
(7.605 ± 0.009 pc)
Absolute magnitude (MV)5.87[8]
Details[9]
Mass0.86 M☉
Radius0.82±0.03 R☉
Luminosity (bolometric)0.46[8] L☉
Surface gravity (log g)4.57±0.10 cgs
Temperature5,172±80 K
Metallicity [Fe/H]−0.01±0.07 dex
Rotation35.0 days[10]
Rotational velocity (v sin i)2.0±1.0 km/s
Age6.3[11] Gyr
Other designations
107 Psc, BD+19°279, GC 2080, HD 10476, HIP 7981, HR 493, SAO 74883, PPM 91014, CCDM J01425+2016A, WDS 01425+2016A, LFT 153, LHS 1287, LTT 10596, NLTT 5685[5][12]
Database references
SIMBADdata

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]

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

  • 107 Piscium in fiction

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.0 2.1 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. ↑ 3.0 3.1 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. doi:10.1086/191373. Bibcode: 1989ApJS...71..245K. 
  4. ↑ 4.0 4.1 4.2 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. ↑ 5.0 5.1 "107 Psc". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=107+Psc. 
  6. ↑ 6.0 6.1 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. doi:10.1086/304453. Bibcode: 1997ApJ...485..789L. 
  7. ↑ 7.0 7.1 Soubiran, C. et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics 616: A7. doi:10.1051/0004-6361/201832795. Bibcode: 2018A&A...616A...7S. 
  8. ↑ 8.0 8.1 8.2 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. ↑ 9.0 9.1 9.2 Fuhrmann, Klaus (2011). "Nearby stars of the Galactic disc and halo - V". Monthly Notices of the Royal Astronomical Society 414 (4): 2893–2922. doi:10.1111/j.1365-2966.2011.18476.x. Bibcode: 2011MNRAS.414.2893F. 
  10. ↑ 10.0 10.1 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, doi:10.1051/0004-6361/201014948, Bibcode: 2010A&A...521A..12M. 
  11. ↑ 11.0 11.1 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, doi:10.1086/591785, Bibcode: 2008ApJ...687.1264M. 
  12. ↑ Entry 01425+2016, The Washington Double Star Catalog , United States Naval Observatory. Accessed on line September 24, 2008.
  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. doi:10.1051/0004-6361/201833377. Bibcode: 2018A&A...619A..81H. 
  14. ↑ Wagman, M. (August 1987), "Flamsteed's Missing Stars", Journal for the History of Astronomy 18 (3): 213, doi:10.1177/002182868701800305, Bibcode: 1987JHA....18..209W 
  15. ↑ Bailer-Jones, C.A.L. et al. (2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics 616: A37. doi:10.1051/0004-6361/201833456. Bibcode: 2018A&A...616A..37B. 
  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. ↑ Radick, Richard R. et al. (March 2018). "Patterns of Variation for the Sun and Sun-like Stars". The Astrophysical Journal 855 (2): 28. doi:10.3847/1538-4357/aaaae3. 75. Bibcode: 2018ApJ...855...75R. 
  18. ↑ Wright, J. T. et al. (August 2008). "The Jupiter Twin HD 154345b". The Astrophysical Journal Letters 683 (1): L63–L66. doi:10.1086/587461. Bibcode: 2008ApJ...683L..63W. 
  19. ↑ 19.0 19.1 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, doi:10.1051/0004-6361/201321673, Bibcode: 2013A&A...555A.104A. 
  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, doi:10.1051/0004-6361/201323056, Bibcode: 2015A&A...574A...6A 

External links



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