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Pi Piscium

This article will address the topic of Pi Piscium from different perspectives, with the aim of providing a comprehensive and in-depth vision of this topic. Its origins, evolution, implications and possible future scenarios will be analyzed, as well as its relevance in today's society. Various research, studies and expert opinions will be examined in order to provide the reader with a complete and up-to-date understanding of Pi Piscium. Additionally, concrete examples and case studies will be presented to exemplify theoretical concepts and foster greater understanding. We hope that this article is useful and interesting to those who wish to deepen their knowledge of Pi Piscium.

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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] (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 mas[1]
Distance114 ± 4 ly
(35 ± 1 pc)
Absolute magnitude (MV)+2.94[2]
Details[3]
A
Mass1.42 M☉
Radius1.68[a] R☉
Luminosity5.45[b] L☉
Surface gravity (log g)4.16 cgs
Temperature6,810 K
Metallicity −0.10 dex
Rotational velocity (v sin i)105.9[2] km/s
Age2.0[5] Gyr
B
Mass0.75 M☉
Radius0.69[a] R☉
Luminosity0.207[b] 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[a] of the Sun's radius. It is radiating 5.5[b] 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[a] times as large, and has 21%[b] 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. ^ a b c d 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:
  2. ^ a b c d Calculated from the equation L = 100.4 • (4.74 − Mbol, where Mbol is the absolute bolometric magnitude. For component A, a value of 2.90 is used, while for B a value of 6.45 is used.

References

  1. ^ a b c d e f 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. ^ a b c d e f 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. ^ a b c d e f g h Fuhrmann, Klaus; Chini, Rolf (January 2019), "On the Secondary of π Piscium", Research Notes of the AAS, 3 (1): 10, Bibcode:2019RNAAS...3...10F, doi:10.3847/2515-5172/aafd39, ISSN 2515-5172.
  4. ^ a b 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.
  5. ^ a b 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.
  6. ^ "pi. Psc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-07-25.{{cite web}}: CS1 maint: postscript (link)
  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, arXiv:1207.0499, Bibcode:2012ApJ...756...46R, doi:10.1088/0004-637X/756/1/46, S2CID 119199829.
  8. ^ 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.
  9. ^ a b "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on 2013-12-03, 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 Archived 2016-03-03 at the Wayback Machine
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