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]
Characteristics
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]
Astrometry
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]
Details
Mass0.83 (0.80 to 0.89)[5] M
Radius0.80 ± 0.06[6] R
Diameter0.80 ± 0.06[6] D
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
SIMBADdata

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]

Naming[edit]

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]

Properties[edit]

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]

References[edit]

  1. 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 Lua error in Module:Citation/CS1 at line 379: attempt to call method 'match' (a nil value).
  2. 2.0 2.1 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. 3.0 3.1 3.2 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.
  4. 4.0 4.1 4.2 4.3 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 Japan 59, #2 (April 2007), pp. 335–356, Bibcode2007PASJ...59..335T.
  5. 5.0 5.1 5.2 5.3 5.4 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. 6.0 6.1 Perrin, M.-N. (1987), "Stellar radius determination from IRAS 12-micron fluxes", Astronomy and Astrophysics 172: 235–240, Bibcode 1987A&A...172..235P.
  7. 7.0 7.1 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. 8.0 8.1 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, arXiv:1007.1132, Bibcode 2010A&A...521A..12M, doi:10.1051/0004-6361/201014948.
  9. 9.0 9.1 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, 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. 12.0 12.1 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, 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


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