104 Tauri

Nowadays, 104 Tauri has become a topic of general interest that covers various areas of daily life. Both on a personal and professional level, 104 Tauri has sparked much debate and generated conflicting opinions. Since his appearance on the public stage, 104 Tauri has captured the attention of millions of people around the world, sparking passionate discussions and deep reflections on his influence on our society. In this article, we will explore the different aspects of 104 Tauri and its impact on our lives, offering a detailed and objective look at this phenomenon that continues to generate controversy.

104 Tauri
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Right ascension 05h 07m 27.00529s[1]
Declination +18° 38′ 42.1815″[1]
Apparent magnitude (V) 4.92[2]
Characteristics
Spectral type G4V[3]
B−V color index 0.64[3]
Astrometry
Radial velocity (Rv)+20.19[3] km/s
Proper motion (μ) RA: +534.73[1] mas/yr
Dec.: +17.93[1] mas/yr
Parallax (π)64.79±0.33 mas[1]
Distance50.3 ± 0.3 ly
(15.43 ± 0.08 pc)
Absolute magnitude (MV)3.75±0.06[4]
Details
Mass1.00+0.03
−0.04[4] M☉
Radius1.63±0.06[4] R☉
Luminosity2.41[5] L☉
Surface gravity (log g)4.06[2] cgs
Temperature5,717[2] K
Metallicity −0.22[2] dex
Rotational velocity (v sin i)10.00[3] km/s
Age10.15[2] Gyr
Other designations
m Tau, 104 Tau, BD+18° 779, GJ 188, HD 32923, HIP 23835, HR 1656, SAO 94332[6]
Database references
SIMBADdata

104 Tauri (104 Tau) is the Flamsteed designation for a star in the equatorial constellation of Taurus. It has an apparent magnitude of 4.92, which is bright enough to be seen with the naked eye. Based upon parallax measurements, this star is located about 50 light-years from the Sun.[1] It is moving further from the Sun with a heliocentric radial velocity of +20 km/s.[3]

This star has a stellar classification of G4 V,[3] which suggests it is an ordinary G-type main-sequence star that is generating energy through hydrogen fusion at its stellar core. It is an estimated 10[2] billion years old and is spinning with a projected rotational velocity of 10 km/s.[3] The star has about the same mass as the Sun, with 1.6 times the Sun's radius.[4] It is radiating 2.4[5] times the Sun's luminosity from its photosphere at an effective temperature of 5,717 K.[2]

104 Tauri appears to have a modest barium enrichment compared to iron. This may indicate that the star had accreted stellar wind of a companion star in the asymptotic giant branch, which has since evolved into a white dwarf.[7]

The star displays convincing evidence for an infrared excess, suggesting the presence of a circumstellar debris disk of dust.[8]

On 24 July 2028, it will be occulted by Venus over Japan, East Siberia and the Pacific Ocean.[9]: 165 

References

  1. ^ a b c d e f van Leeuwen, F. (November 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 e f g Ramírez, I.; et al. (February 2013), "Oxygen abundances in nearby FGK stars and the galactic chemical evolution of the local disk and halo", The Astrophysical Journal, 764 (1): 78, arXiv:1301.1582, Bibcode:2013ApJ...764...78R, doi:10.1088/0004-637X/764/1/78, S2CID 118751608.
  3. ^ a b c d e f g White, Russel J.; et al. (June 2007), "High-Dispersion Optical Spectra of Nearby Stars Younger Than the Sun", The Astronomical Journal, 133 (6): 2524–2536, arXiv:0706.0542, Bibcode:2007AJ....133.2524W, doi:10.1086/514336, S2CID 122854.
  4. ^ a b c d Bernkopf, Jan; Fuhrmann, Klaus (June 2006), "Local subgiants and time-scales of disc formation", Monthly Notices of the Royal Astronomical Society, 369 (2): 673–676, Bibcode:2006MNRAS.369..673B, doi:10.1111/j.1365-2966.2006.10326.x.
  5. ^ a b 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. ^ "m Tau -- Double or multiple star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2013-08-12.
  7. ^ Fuhrmann, K.; Chini, R.; Kaderhandt, L.; Chen, Z.; Lachaume, R. (2017-07-21). "The barium-to-iron enrichment versus age relation of ancient disc stars". Monthly Notices of the Royal Astronomical Society. 471 (3). Oxford University Press (OUP): 3768–3774. Bibcode:2017MNRAS.471.3768F. doi:10.1093/mnras/stx1848. ISSN 0035-8711.
  8. ^ Holmes, E. K.; et al. (June 2003), "A Survey of Nearby Main-Sequence Stars for Submillimeter Emission", The Astronomical Journal, 125 (6): 3334–3343, Bibcode:2003AJ....125.3334H, doi:10.1086/375202.
  9. ^ Meeus, Jan (2002). "Mutual occultations of planets". More Mathematical Astronomy Morsels (PDF). pp. 174–185. ISBN 0943396743.


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