107 Piscium

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107 Piscium
Observation data
Epoch J2000.0        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  mas [1]
Distance 24.80 ± 0.03  ly
(7.605 ± 0.009  pc)
Absolute magnitude  (MV)5.87 [8]
Details [9]
Mass 0.86  M☉
Radius 0.82±0.03  R☉
Luminosity (bolometric)0.46 [8]   L☉
Surface gravity (log g)4.57±0.10  cgs
Temperature 5,172±80  K
Metallicity [Fe/H]−0.01±0.07  dex
Rotation 35.0 days [10]
Rotational velocity (v sin i)2.0±1.0 km/s
Age 6.3 [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
SIMBAD data

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]

Contents

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 2 3 4 5 6 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. 1 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. 1 2 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. 1 2 3 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. 1 2 "107 Psc". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved September 24, 2008.
  6. 1 2 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. 1 2 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. 1 2 3 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 Japan59, #2 (April 2007), pp. 335–356, Bibcode:2007PASJ...59..335T.
  9. 1 2 3 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. 1 2 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. 1 2 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. ↑ 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. ↑ 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. ↑ 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. ↑ 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. ↑ 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. Bibcode:2018ApJ...855...75R. doi: 10.3847/1538-4357/aaaae3 . 75.
  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. 1 2 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. ↑ 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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