Tau3 Eridani

In today's world, Tau3 Eridani has become a topic of great relevance and interest to a wide spectrum of society. On both a personal and professional level, Tau3 Eridani has made a significant impact on our lives. In order to better understand this phenomenon and offer a broad and detailed vision, in this article we will explore different aspects related to Tau3 Eridani. From its origins to its influence on the present, including its future implications, we will delve into an exhaustive analysis that seeks to shed light on this very important topic. By exploring relevant studies, testimonials, and data, we hope to provide a comprehensive and enriching view of Tau3 Eridani that our readers may find useful and enlightening.

For other star systems with this Bayer designation, see Tau Eridani.
τ3 Eridani
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Eridanus
Right ascension 03h 02m 23.49939s[1]
Declination −23° 37′ 28.0936″[1]
Apparent magnitude (V) 4.10[2]
Characteristics
Spectral type A3 IV-V[3]
U−B color index +0.08[2]
B−V color index +0.16[2]
Astrometry
Radial velocity (Rv)−9.8[4] km/s
Proper motion (μ) RA: −147.25[1] mas/yr
Dec.: −55.28[1] mas/yr
Parallax (π)36.80±0.18 mas[1]
Distance88.6 ± 0.4 ly
(27.2 ± 0.1 pc)
Absolute magnitude (MV)+1.91[5]
Details
Mass1.78[6] M☉
Radius1.9[7] R☉
Luminosity13.7[8] L☉
Surface gravity (log g)4.17[6] cgs
Temperature8,251±281[6] K
Metallicity −0.21[3] dex
Rotational velocity (v sin i)133[9] km/s
Age476[6] Myr
Other designations
τ3 Eridani, τ3 Eri, 11 Eridani, CD-24° 1387, HD 18978, HIP 14146, HR 919, SAO 168249.[10]
Database references
SIMBADdata

Tau3 Eridani, Latinized from τ3 Eridani, is a star in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 4.10.[2] Using the parallax method,[1] the distance to this star can be estimated as 88.6 light years. In 2001 it was reported as a candidate Vega-like star, meaning it appears to radiate an infrared excess from an orbiting circumstellar disk.[11] However, this has not been confirmed.[12]

This is an A-type star with a stellar classification of A3 IV-V.[3] The luminosity class of IV-V indicates the spectrum displays traits intermediate between a main sequence and subgiant star. It is around 476[6] million years old and is spinning rapidly with a projected rotational velocity of 133 km/s.[9] This is creating an equatorial bulge that might be 7% wider than the polar radius.[13] Tau3 Eridani has 178%[6] of the Sun's mass and nearly double the radius of the Sun.[7] The star shines with 13.7 times the solar luminosity from an outer atmosphere at an effective temperature of 8,251 K.[6]

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 Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data, SIMBAD, Bibcode:1986EgUBV........0M.
  3. ^ a b c 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. ^ Wilson, R. E. (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Carnegie Institute of Washington, D.C., Bibcode:1953GCRV..C......0W.
  5. ^ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  6. ^ a b c d e f g David, Trevor J.; Hillenbrand, Lynne A. (May 2015), "The Ages of Early-type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 38, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607, 146.
  7. ^ a b Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics", Astronomy and Astrophysics, 367 (2): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451, S2CID 425754.
  8. ^ McDonald, I.; et al. (2012), "Fundamental Parameters and Infrared Excesses of Hipparcos Stars", Monthly Notices of the Royal Astronomical Society, 427 (1): 343–57, arXiv:1208.2037, Bibcode:2012MNRAS.427..343M, doi:10.1111/j.1365-2966.2012.21873.x, S2CID 118665352.
  9. ^ a b Royer, F.; et al. (February 2007), "Rotational velocities of A-type stars. III. Velocity distributions", Astronomy and Astrophysics, 463 (2): 671–682, arXiv:astro-ph/0610785, Bibcode:2007A&A...463..671R, doi:10.1051/0004-6361:20065224, S2CID 18475298.
  10. ^ "tau03 Eri". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-10-13.{{cite web}}: CS1 maint: postscript (link)
  11. ^ Song, Inseok; et al. (January 2001), "Ages of A-Type Vega-like Stars from uvbyβ Photometry", The Astrophysical Journal, 546 (1): 352–357, arXiv:astro-ph/0010102, Bibcode:2001ApJ...546..352S, doi:10.1086/318269, S2CID 18154947.
  12. ^ Gáspár, András; et al. (May 2013), "The Collisional Evolution of Debris Disks", The Astrophysical Journal, 768 (1): 29, arXiv:1211.1415, Bibcode:2013ApJ...768...25G, doi:10.1088/0004-637X/768/1/25, S2CID 119295265, 25.
  13. ^ Van Belle, Gerard T. (2012), "Interferometric observations of rapidly rotating stars", The Astronomy and Astrophysics Review, 20 (1): 51, arXiv:1204.2572, Bibcode:2012A&ARv..20...51V, doi:10.1007/s00159-012-0051-2, S2CID 119273474.