Tau6 Eridani

In this article, we will explore the fascinating world of Tau6 Eridani and its impact on today's society. From its origins to its relevance today, Tau6 Eridani has been a topic of debate and reflection in various fields, whether in popular culture, politics, science or technology. Throughout history, Tau6 Eridani has had a significant influence on the way people interact with each other and the environment around them. Through this article, we will examine in detail the different aspects that make Tau6 Eridani such a relevant and constantly evolving topic.

For other star systems with this Bayer designation, see Tau Eridani.
τ6 Eridani
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Eridanus
Right ascension 03h 46m 50.88819s[1]
Declination −23° 14′ 59.0046″[1]
Apparent magnitude (V) 4.22[2]
Characteristics
Spectral type F5IV-V[3]
U−B color index −0.03[2]
B−V color index +0.43[2]
Astrometry
Radial velocity (Rv)8.0±0.8[4] km/s
Proper motion (μ) RA: −158.84[1] mas/yr
Dec.: −528.95[1] mas/yr
Parallax (π)56.73±0.19 mas[1]
Distance57.5 ± 0.2 ly
(17.63 ± 0.06 pc)
Absolute magnitude (MV)2.98[5]
Details
Mass1.35[4] M☉
Radius1.80+0.08
−0.03[6] R☉
Luminosity5.47±0.06[6] L☉
Surface gravity (log g)4.21±0.13[4] cgs
Temperature6,584+47
−144[6] K
Metallicity −0.03±0.11[4] dex
Rotational velocity (v sin i)16.25[7] km/s
Age2.0[4] Gyr
Other designations
τ6 Eri, 27 Eridani, CD−23°1565, FK5 140, GC 168827, HD 23754, HIP 17651, HR 1173, SAO 101600[8]
Database references
SIMBADdata

Tau6 Eridani, Latinized from τ6 Eridani, is a single[9] star in the equatorial constellation of Eridanus, located near the constellation border with Fornax. It has a yellow-white hue with an apparent visual magnitude of 4.22,[2] which is bright enough to be seen with the naked eye. Based upon parallax measurements, the distance to this star is around 57.5 light years.[1] It is drifting further away with a radial velocity of +8 km/s.[4]

The spectrum of Tau6 Eridani matches a stellar classification of F5IV-V,[3] indicating it is an F-type star that shows traits of both a main sequence star and a subgiant. It has an estimated 135%[4] of the Sun's mass and about 1.8 time the radius of the Sun.[6] The star is radiating 5.5[6] times the luminosity of the Sun at an effective temperature of 6,508 K,[4] and it does not display any surface magnetic activity.[7] The star has been examined for infrared excess emission that could indicate the presence of circumstellar matter, but none has been detected.[10]

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 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. ^ a b c d e f g h Kordopatis, G.; Gilmore, G.; Steinmetz, M.; Boeche, C.; Seabroke, G. M.; Siebert, A.; Zwitter, T.; Binney, J.; et al. (November 2013), "The Radial Velocity Experiment (RAVE): Fourth Data Release", The Astronomical Journal, 146 (5): 36, arXiv:1309.4284, Bibcode:2013AJ....146..134K, doi:10.1088/0004-6256/146/5/134, S2CID 119221010, 134.
  5. ^ Reiners, Ansgar (January 2006), "Rotation- and temperature-dependence of stellar latitudinal differential rotation", Astronomy and Astrophysics, 446 (1): 267–277, arXiv:astro-ph/0509399, Bibcode:2006A&A...446..267R, doi:10.1051/0004-6361:20053911, S2CID 8642707
  6. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  7. ^ a b Martínez-Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter" (PDF), Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725, S2CID 43455849, archived from the original (PDF) on 2017-09-22, retrieved 2018-11-04.
  8. ^ "* tau06 Eri". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-10-13.
  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. ^ Weinberger, Alycia J.; Bryden, Geoff; Kennedy, Grant M.; Roberge, Aki; Defrère, Denis; Hinz, Philip M.; Millan-Gabet, Rafael; Rieke, George; et al. (February 2015), "Target Selection for the LBTI Exozodi Key Science Program", The Astrophysical Journal Supplement Series, 216 (2): 8, arXiv:1501.01319, Bibcode:2015ApJS..216...24W, doi:10.1088/0067-0049/216/2/24, S2CID 38713562, 24.