75 Tauri

Nowadays, 75 Tauri is a topic that arouses great interest and debate in today's society. Its relevance ranges from personal aspects to global issues, and its impact is evident in different areas. As time goes on, 75 Tauri continues to be a topical topic that continues to generate controversy. From the perspective of research and analysis, it is necessary to delve into the different aspects covered by 75 Tauri to understand its scope and importance in the contemporary world. In this article, we will delve into the most relevant aspects of 75 Tauri and analyze its influence on today's society.

75 Tauri
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Taurus
Right ascension 04h 28m 26.37004s[1]
Declination +16° 21′ 34.8231″[1]
Apparent magnitude (V) 4.96[2]
Characteristics
Spectral type K1 IIIb[2]
B−V color index 1.137[3]
Astrometry
Radial velocity (Rv)+16.24±0.20[4] km/s
Proper motion (μ) RA: +7.91[1] mas/yr
Dec.: +18.14[1] mas/yr
Parallax (π)17.47±0.42 mas[1]
Distance187 ± 4 ly
(57 ± 1 pc)
Absolute magnitude (MV)1.18[3]
Details[3]
Mass1.53±0.23 M☉
Radius11[5] R☉
Luminosity40.74+2.02
−1.92 L☉
Surface gravity (log g)2.81±0.28 cgs
Temperature4,697±60 K
Metallicity −0.08±0.11 dex
Rotational velocity (v sin i)2.5[5] km/s
Age2.7+1.0
−1.5 Gyr
Other designations
75 Tau, BD+16° 605, HD 28292, HIP 20877, HR 1407, SAO 93950, WDS J04284+1622AB[6]
Database references
SIMBADdata

75 Tauri is a single,[7] orange-hued star in the zodiac of constellation Taurus. It is a dim star but visible to the naked eye with an apparent visual magnitude of 4.96.[2] Based upon an annual parallax shift of 17.47 mas as seen from Earth's orbit, it is located around 187 light years away. Due to its position near the ecliptic, it is subject to lunar occultations.[8] The star is moving further from the Sun with a heliocentric radial velocity of +16 km/s.[4]

The stellar classification of 75 Tauri is K1 IIIb,[2] indicating it is an aging giant star that has exhausted the supply of hydrogen at its core. At the estimated age of roughly 2.7 billion years,[3] this has become a red clump star that is generating energy through helium fusion in its core region.[9] The star has 1.5 times the mass of the Sun and has expanded to 11 times the Sun's radius. It is radiating 41 times the Sun's luminosity from its enlarged photosphere at an effective temperature of around 4,697 K.[3]

References

  1. ^ a b c d e 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 Keenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245, Bibcode:1989ApJS...71..245K, doi:10.1086/191373.
  3. ^ a b c d e Da Silva, Ronaldo; et al. (2015), "Homogeneous abundance analysis of FGK dwarf, subgiant, and giant stars with and without giant planets", Astronomy & Astrophysics, 580: A24, arXiv:1505.01726, Bibcode:2015A&A...580A..24D, doi:10.1051/0004-6361/201525770, S2CID 119216425.
  4. ^ a b de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics, 546: 14, arXiv:1208.3048, Bibcode:2012A&A...546A..61D, doi:10.1051/0004-6361/201219219, S2CID 59451347, A61.
  5. ^ a b Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209, S2CID 121883397.
  6. ^ "75 Tau". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2018-02-22.
  7. ^ 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.
  8. ^ Evans, D. S.; Edwards, D. A. (August 1981), "Photoelectric observations of lunar occultations. XII", Astronomical Journal, 86: 1277−1287, Bibcode:1981AJ.....86.1277E, doi:10.1086/113008.
  9. ^ Tautvaišienė, G.; et al. (December 2010), "C, N and O abundances in red clump stars of the Milky Way", Monthly Notices of the Royal Astronomical Society, 409 (3): 1213–1219, arXiv:1007.4064, Bibcode:2010MNRAS.409.1213T, doi:10.1111/j.1365-2966.2010.17381.x, S2CID 119182458.