Tau7 Eridani

In this article we will explore the different facets of Tau7 Eridani and its impact on modern society. From its beginnings to its current evolution, Tau7 Eridani has left an indelible mark on various aspects of our lives. We will analyze its influence on culture, economy, technology and politics, seeking to understand its relevance in the contemporary world. Through the collection of data, testimonials and expert opinions, we aim to offer a comprehensive view of Tau7 Eridani and its role today.

For other star systems with this Bayer designation, see Tau Eridani.
τ7 Eridani
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Eridanus
Right ascension 03h 47m 39.65058s[1]
Declination −23° 52′ 28.8352″[1]
Apparent magnitude (V) 5.235[2]
Characteristics
Spectral type A3 Vs[3]
U−B color index +0.168[2]
B−V color index +0.067[2]
Astrometry
Radial velocity (Rv)28.4±0.5[4] km/s
Proper motion (μ) RA: +47.46[1] mas/yr
Dec.: +49.10[1] mas/yr
Parallax (π)13.00±0.28 mas[1]
Distance251 ± 5 ly
(77 ± 2 pc)
Absolute magnitude (MV)+0.81[5]
Details
τ7 Eri A
Mass2.03[6] M☉
Luminosity37.6[7] L☉
Surface gravity (log g)3.86±0.2[8] cgs
Temperature8,740±200[8] K
Rotational velocity (v sin i)18[8] km/s
Age387[6] Myr
Other designations
τ7 Eridani, τ7 Eri, 28 Eridani, CD−24° 1877, HD 23878, HIP 17717, HR 1181, SAO 168836.[9]
Database references
SIMBADdata

Tau7 Eridani is a solitary star in the constellation Eridanus. It is visible to the naked eye with an apparent visual magnitude of 5.235.[2] Using the parallax method, the distance to this star can be estimated as around 251 light years.[1]

This is an A-type main sequence star with a stellar classification of A3 Vs,[3] where the 's' indicates it has narrow absorption lines. It may be a chemically peculiar Am star, which means it displays unusual abundances of certain elements in its surface layers. Tau7 Eridani appears to be a low amplitude variable that displays slight fluctuations in luminosity over a period of 7.17 days. It is slowly rotating with a projected rotational velocity of 18 km/s,[8] and is around 387 million years old.[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 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.
  3. ^ a b Abt, Helmut A.; Morrell, Nidia I. (July 1995), "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars", Astrophysical Journal Supplement, 99: 135, Bibcode:1995ApJS...99..135A, doi:10.1086/192182.
  4. ^ De Bruijne, J. H. J.; Eilers, A.-C. (2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: A61, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347.
  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 David, Trevor J.; Hillenbrand, Lynne A. (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): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
  7. ^ 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.
  8. ^ a b c d Khalack, V.; LeBlanc, F. (July 2015), "Project VeSElkA: Analysis of Balmer Line Profiles of Slowly Rotating Chemically Peculiar Stars", The Astronomical Journal, 150 (1): 10, arXiv:1505.08158, Bibcode:2015AJ....150....2K, doi:10.1088/0004-6256/150/1/2, S2CID 118283214, 2.
  9. ^ "tau07 Eri". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-10-13.{{cite web}}: CS1 maint: postscript (link)