Astronomy:Pi Piscium

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Short description: Binary star in the constellation Pisces
Pi Piscium
Location of π Piscium (circled)
Observation data
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] (5.56 + 9.56)[3]
Characteristics
Spectral type F0 V[4] + KV[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[1] mas
Distance114 ± 4 ly
(35 ± 1 pc)
Absolute magnitude (MV)+2.94[2]
Details[3]
A
Mass1.42 M☉
Radius1.68[lower-alpha 1] R☉
Luminosity5.45[lower-alpha 2] L☉
Surface gravity (log g)4.16 cgs
Temperature6,810 K
Metallicity [Fe/H]−0.10 dex
Rotational velocity (v sin i)105.9[2] km/s
Age2.0[5] Gyr
B
Mass0.75 M☉
Radius0.69[lower-alpha 1] R☉
Luminosity0.207[lower-alpha 2] L☉
Temperature4,700 K
Other designations
π Psc, 102 Piscium, BD+11°205, FK5 1046, GC 1954, HD 9919, HIP 7535, HR 463, SAO 92536, PPM 117498[6]
Database references
SIMBADdata

Pi Piscium (π Piscium) is a spectroscopic binary[3] 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 114 light years distant. It is a member of the thin disk population of the Milky Way.[7]

The primary, of apparent magnitude 5.56,[3] is an ordinary F-type main-sequence star with a stellar classification of F0 V.[4] At the estimated age of two billion years,[5] it is about 55% of the way through its main sequence lifetime[8] and still has a relatively high rate of spin with a projected rotational velocity of 105.9 km/s.[2] The star has 1.42 times the mass of the Sun and 1.68[lower-alpha 1] of the Sun's radius. It is radiating 5.5[lower-alpha 2] times the Sun's luminosity at an effective temperature of 6,810 K.[3] At that temperature, Pi Piscium A has a yellow-white hue, as many F-type stars.[9]

The secondary, of apparent magnitude 9.56, is a K-dwarf star. It is 0.75 times as massive than the Sun, 0.69[lower-alpha 1] times as large, and has 21%[lower-alpha 2] of the luminosity. Its effective temperature is 4,700 K,[3] giving it an orange hue typical of K-type stars.[9]

Analysis of its motion suggest Pi Piscium may be a member of the Ursa Major association, but higher-quality observations are needed to confirm this.[3]

Naming

In Chinese, 右更 (Yòu Gèng), meaning Official in Charge of the Pasturing, 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.)[10]

Notes

  1. ↑ 1.0 1.1 1.2 1.3 Calculated, using the Stefan-Boltzmann law and the star's effective temperature and luminosity, with respect to the solar nominal effective temperature of 5,772 K:(5,7726,810)4⋅5.45=1.68 R⊙.(5,7724,700)4⋅0.207=0.69 R⊙.
  2. ↑ 2.0 2.1 2.2 2.3 Calculated from the equation L = 100.4Slovene pronunciation: [{{{1}}}]Thai pronunciation: [{{{1}}}]Neukirch, Jürgen; Schmidt, Alexander; Wingberg, Kay (2000), Cohomology of Number Fields, Grundlehren der Mathematischen Wissenschaften, 323, Berlin: Springer-Verlag, ISBN 978-3-540-66671-4 Template:ScribuntoPersian pronunciation: [{{{1}}}]{| class="wikitable" width="100%"

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References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Paunzen, E. et al. (July 2014), "Investigating the possible connection between λ Bootis stars and intermediate Population II type stars", Astronomy & Astrophysics 567: 8, doi:10.1051/0004-6361/201423817, A67, Bibcode: 2014A&A...567A..67P. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 Fuhrmann, Klaus; Chini, Rolf (January 2019), "On the Secondary of π Piscium" (in en), Research Notes of the AAS 3 (1): 10, doi:10.3847/2515-5172/aafd39, ISSN 2515-5172, Bibcode: 2019RNAAS...3...10F. 
  4. ↑ 4.0 4.1 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, doi:10.1086/129562, Bibcode: 1974PASP...86...70C. 
  5. ↑ 5.0 5.1 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, doi:10.1051/0004-6361/200811191, Bibcode: 2009A&A...501..941H. 
  6. ↑ "pi. Psc". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=pi.+Psc. 
  7. ↑ 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, doi:10.1088/0004-637X/756/1/46, Bibcode: 2012ApJ...756...46R. 
  8. ↑ Zorec, J.; Royer, F. (January 2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy & Astrophysics 537: A120, doi:10.1051/0004-6361/201117691, Bibcode: 2012A&A...537A.120Z. 
  9. ↑ 9.0 9.1 "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html, retrieved 2012-01-16 
  10. ↑ (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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