 | |
| 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] |
| Distance | 59.6 ± 0.3 ly (18.28 ± 0.09 pc) |
| Absolute magnitude (MV) | 3.58[4] |
| Details | |
| 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 | |
| Database references | |
| SIMBAD | data |
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]
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CONSTELAȚIA VĂRSĂTOR SAU PAHARNIC - AQUARIUS - VĂRSĂTORUL
Transcription
The Aquarius is an ecliptic constellation, best visible during the eveneings of October. The constellation is situated in a sky area often called „the sea" due to the abundance of constellations with names closely linked with water. It is surrounded by constellation Pisces, Cetus, Sculptor, Piscis Austrinus, Capricorn, Equuleus , Delphinus and Pegasus. The brightest star of the constellation is Sadalsuud, the name coming from Arabic language and meaning „the luckiest fortunate man" in an aproximate translation. Romanians have the same name for this constellation, and the story of the character come from Greek mythology, where it is identified with Gabymede, the Gods cup-bearer.
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
- ^ 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.
- ^ a b c d Gutierrez-Moreno, Adelina; et al. (1966), "A System of photometric standards", Publications of the Department of Astronomy University of Chile, 1, Publicaciones Universidad de Chile, Department de Astronomy: 1–17, Bibcode:1966PDAUC...1....1G.
- ^ 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/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
- ^ a b c d e 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.
- ^ 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:1002.4268, Bibcode:2010MNRAS.405.1907B, doi:10.1111/j.1365-2966.2010.16575.x, S2CID 118495267.
- ^ 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:1502.07100, Bibcode:2015A&A...579A..20M, doi:10.1051/0004-6361/201525764, S2CID 118434947, A20.
- ^ 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.
- ^ "tau PsA -- High proper-motion Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2017-05-17.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ (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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This page was last edited on 24 February 2023, at 17:57