Tau Piscis Austrini

From Wikipedia, the free encyclopedia
Jump to: navigation, search
Tau Piscis Austrini
Diagram showing star positions and boundaries of the Piscis Austrinus constellation and its surroundings
Cercle rouge 100%.svg
Location of τ Piscis Austrini (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Piscis Austrinus
Right ascension 22h 10m 08.78048s[1]
Declination −32° 32′ 54.2687″[1]
Apparent magnitude (V) +4.945[2]
Spectral type F6 V[3]
U−B color index +0.031[2]
B−V color index +0.488[2]
Proper motion (μ) RA: +428.96[1] mas/yr
Dec.: +13.35[1] mas/yr
Parallax (π) 54.71 ± 0.28[1] mas
Distance 59.6 ± 0.3 ly
(18.28 ± 0.09 pc)
Absolute magnitude (MV) 3.58[4]
Mass 1.34±0.13[5] M
Radius 1.45±0.04[5] R
Luminosity 2.82±0.09[5] L
Surface gravity (log g) 4.11[6] cgs
Temperature 6,324[4] K
Metallicity [Fe/H] −0.01[6] dex
Rotational velocity (v sin i) 14.1±0.7[4] km/s
Age 1.3[7] Gyr
Other designations
τ PsA, 15 Piscis Austrini, CPD−33° 6227, HD 210302, HIP 109422, HR 8447, SAO 213602[8]
Database references

Tau Piscis Austrini (τ Piscis Austrini) is a solitary,[9] yellow-white hued star in the southern constellation of Piscis Austrinus. It is visible to the naked eye with an apparent visual magnitude of +4.9.[2] Based upon an annual parallax shift of 54.71 mas as seen from the Earth,[1] the star is located 59.6 light years from the Sun.

This is an F-type main sequence star with a stellar classification of F6 V.[3] It is about 1.3[7] billion years old with a projected rotational velocity of 14[4] km/s and exhibits a low level of activity.[10] The star has an estimated 1.34 times the mass of the Sun and 1.45 times the Sun's radius.[5] It is radiating 2.82[5] times the solar luminosity from its photosphere at an effective temperature of 6,324 K.[4] This star is a candidate for hosting a debris disk, as it displayed an initial near infrared excess that faded with further observations.[11]


In Chinese, 天錢 (Tiān Qián), meaning Celestial Money, refers to an asterism consisting of refers to an asterism consisting of τ Piscis Austrini, 13 Piscis Austrini, θ Piscis Austrini, ι Piscis Austrini and μ Piscis Austrini. Consequently, τ Piscis Austrini itself is known as 天錢五 (Tiān Qián wǔ, English: the Fifth Star of Celestial Money.)[12]


  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:0708.1752Freely accessible, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357. 
  2. ^ a b c d Gutierrez-Moreno, Adelina; et al. (1966), A System of photometric standards, 1, Publicaciones Universidad de Chile, Department de Astronomy, pp. 1–17, Bibcode:1966PDAUC...1....1G. 
  3. ^ a b Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770Freely accessible, Bibcode:2006AJ....132..161G, doi:10.1086/504637. 
  4. ^ a b c d e Ammler-von Eiff, M.; Reiners, A. (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: 31, arXiv:1204.2459Freely accessible, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, A116. 
  5. ^ a b c d e Bruntt, H.; et al. (July 2010), "Accurate fundamental parameters for 23 bright solar-type stars", Monthly Notices of the Royal Astronomical Society, 405 (3): 1907–1923, arXiv:1002.4268Freely accessible, Bibcode:2010MNRAS.405.1907B, doi:10.1111/j.1365-2966.2010.16575.x. 
  6. ^ a b Maldonado, J.; et al. (July 2015), "Searching for signatures of planet formation in stars with circumstellar debris discs", Astronomy & Astrophysics, 579: 41, arXiv:1502.07100Freely accessible, Bibcode:2015A&A...579A..20M, doi:10.1051/0004-6361/201525764, A20. 
  7. ^ 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:0811.3982Freely accessible, Bibcode:2009A&A...501..941H, doi:10.1051/0004-6361/200811191. 
  8. ^ "tau PsA -- High proper-motion Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-05-17. 
  9. ^ 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:0806.2878Freely accessible, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x. 
  10. ^ Meunier, N.; et al. (September 2012), "Comparison of different exoplanet mass detection limit methods using a sample of main-sequence intermediate-type stars", Astronomy & Astrophysics, 545: 16, arXiv:1207.4329Freely accessible, Bibcode:2012A&A...545A..87M, doi:10.1051/0004-6361/201219163, A87. 
  11. ^ Ertel, S.; et al. (October 2016), "A near-infrared interferometric survey of debris-disc stars. V. PIONIER search for variability", Astronomy & Astrophysics, 595: 6, arXiv:1608.05731Freely accessible, Bibcode:2016A&A...595A..44E, doi:10.1051/0004-6361/201527721, A44. 
  12. ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 5 日