Tau Piscis Austrini
Diagram showing star positions and boundaries of the Piscis Austrinus constellation and its surroundings
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]
Characteristics
Spectral type F6 V[3]
U−B color index +0.031[2]
B−V color index +0.488[2]
Astrometry
Proper motion (μ) RA: +428.96[1] mas/yr
Dec.: +13.35[1] mas/yr
Parallax (π)54.71 ± 0.28 mas[1]
Distance59.6 ± 0.3 ly
(18.28 ± 0.09 pc)
Absolute magnitude (MV)3.58[4]
Details
Mass1.34±0.13[5] M☉
Radius1.45±0.04[5] R☉
Luminosity2.82±0.09[5] L☉
Surface gravity (log g)4.11[6] cgs
Temperature6,324[4] K
Metallicity [Fe/H]−0.01[6] dex
Rotational velocity (v sin i)14.1±0.7[4] km/s
Age1.3[7] Gyr
Other designations
τ PsA, 15 Piscis Austrini, CPD−33° 6227, HD 210302, HIP 109422, HR 8447, SAO 213602[8]
Database references
SIMBADdata

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]

Naming

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, the Chinese name for τ Piscis Austrini itself is 天錢五 (Tiān Qián wǔ, English: the Fifth Star of Celestial Money.)[12]

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 Gutierrez-Moreno, Adelina; et al. (1966), "A System of photometric standards", Publications of the Department of Astronomy University of Chile, Publicaciones Universidad de Chile, Department de Astronomy, 1: 1–17, Bibcode:1966PDAUC...1....1G.
  3. 1 2 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/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
  4. 1 2 3 4 5 Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, S2CID 53666672.
  5. 1 2 3 4 5 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:1002.4268, Bibcode:2010MNRAS.405.1907B, doi:10.1111/j.1365-2966.2010.16575.x, S2CID 118495267.
  6. 1 2 Maldonado, J.; et al. (July 2015), "Searching for signatures of planet formation in stars with circumstellar debris discs", Astronomy & Astrophysics, 579: 41, arXiv:1502.07100, Bibcode:2015A&A...579A..20M, doi:10.1051/0004-6361/201525764, S2CID 118434947, A20.
  7. 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.
  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:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
  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:1207.4329, Bibcode:2012A&A...545A..87M, doi:10.1051/0004-6361/201219163, S2CID 59138448, 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:1608.05731, Bibcode:2016A&A...595A..44E, doi:10.1051/0004-6361/201527721, S2CID 7277663, 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
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