Pi Piscium
Location of π Piscium (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Pisces
Right ascension 01h 37m 05.91523s[1]
Declination +12° 08′ 29.5186″[1]
Apparent magnitude (V) 5.60[2]
Characteristics
Spectral type F0 V[3]
Astrometry
Radial velocity (Rv)−1.0[2] km/s
Proper motion (μ) RA: −77.29[1] mas/yr
Dec.: +9.13[1] mas/yr
Parallax (π)28.50 ± 0.97 mas[1]
Distance114 ± 4 ly
(35 ± 1 pc)
Absolute magnitude (MV)+2.94[2]
Details
Mass1.51±0.02[4] M☉
Luminosity6.3[4] L☉
Surface gravity (log g)4.00[2] cgs
Temperature6,850[2] K
Metallicity [Fe/H]−0.45±0.05[5] dex
Rotational velocity (v sin i)105.9[2] km/s
Age2.0[6] Gyr
Other designations
π Psc, 102 Piscium, BD+11° 205, FK5 1046, GC 1954, HD 9919, HIP 7535, HR 463, SAO 92536, PPM 117498[7]
Database references
SIMBADdata

Pi Piscium (π Piscium) is a solitary,[8] yellow-white hued star in the zodiac constellation of Pisces. It is faintly visible to the naked eye, having an apparent visual magnitude of 5.60.[2] Based upon an annual parallax shift of 28.50 mas as seen from Earth,[1] it is located about 1114 light years from the Sun. It is a member of the thin disk population of the Milky Way.[5]

This is an ordinary F-type main-sequence star with a stellar classification of F0 V.[3] At the estimated age of two billion years,[6] it is about 55% of the way through its main sequence lifetime[4] and still has a relatively high rate of spin with a projected rotational velocity of 105.9 km/s.[2] The star has 1.5[4] times the mass of the Sun and is radiating 6.3[4] times the Sun's luminosity at an effective temperature of 6,850 K.[2]

Naming

In Chinese, 右更 (Yòu Gèng), meaning Official in Charge of the Pasturing, refers to an asterism consisting of refers to an asterism consisting of π Piscium, η Piscium, ρ Piscium, ο Piscium and 104 Piscium. Consequently, the Chinese name for π Piscium itself is 右更三 (Yòu Gèng sān, English: the Third Star of Official in Charge of the Pasturing.)[9]

References

  1. 1 2 3 4 5 6 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  2. 1 2 3 4 5 6 7 8 9 Paunzen, E.; et al. (July 2014), "Investigating the possible connection between λ Bootis stars and intermediate Population II type stars", Astronomy & Astrophysics, 567: 8, arXiv:1406.3936, Bibcode:2014A&A...567A..67P, doi:10.1051/0004-6361/201423817, S2CID 56332289, A67.
  3. 1 2 Cowley, Anne; Fraquelli, Dorothy (February 1974), "MK Spectral Types for Some Bright F Stars", Publications of the Astronomical Society of the Pacific, 86 (509): 70, Bibcode:1974PASP...86...70C, doi:10.1086/129562.
  4. 1 2 3 4 5 Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691, S2CID 55586789.
  5. 1 2 Ramírez, I.; et al. (September 2012), "Lithium Abundances in nearby FGK Dwarf and Subgiant Stars: Internal Destruction, Galactic Chemical Evolution, and Exoplanets", The Astrophysical Journal, 756 (1): 46, arXiv:1207.0499, Bibcode:2012ApJ...756...46R, doi:10.1088/0004-637X/756/1/46, S2CID 119199829.
  6. 1 2 Holmberg, J.; et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics, 501 (3): 941–947, arXiv:0811.3982, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191, S2CID 118577511.
  7. ↑ "pi. Psc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-07-25.{{cite web}}: CS1 maint: postscript (link)
  8. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society, 389 (2): 869–879, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  9. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 19 日
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