Gliese 673

In today's world, Gliese 673 has become a topic of great relevance and interest. Over time, Gliese 673 has proven to be a topic that leaves no one indifferent, generating debates, conflicting opinions and endless reflections. The importance of Gliese 673 lies in its impact on various aspects of daily life, from politics to popular culture. Likewise, Gliese 673 has been the subject of study and research, giving rise to numerous advances and discoveries that have revolutionized our understanding of the world around us. In this article, we will explore in depth the impact of Gliese 673 and its influence on different spheres of society.

Gliese 673
Gliese 673 is located in the constellation Ophiuchus.
Gliese 673 is located in the constellation Ophiuchus.
  Gliese 673
Location of Gliese 673 in the constellation Ophiuchus

Observation data
Epoch J2000      Equinox J2000
Constellation Ophiuchus
Right ascension 17h 25m 45.23243s[1]
Declination +02° 06′ 41.1237″[1]
Apparent magnitude (V) 7.492[2]
Characteristics
Spectral type K7V[2]
U−B color index 1.261[2]
B−V color index 1.373[2]
Astrometry
Radial velocity (Rv)−23.87±0.12[1] km/s
Proper motion (μ) RA: −580.325 mas/yr[1]
Dec.: −1,184.737 mas/yr[1]
Parallax (π)129.6459±0.0175 mas[1]
Distance25.157 ± 0.003 ly
(7.713 ± 0.001 pc)
Absolute magnitude (MV)8.06[2]
Details
Radius0.564±0.068[3] R☉
Surface gravity (log g)4.70[4] cgs
Temperature4,030[3] K
Metallicity −0.20[4] dex
Rotation11.94 days[5]
Age205±21[5] Myr
Other designations
BD+02 3312, GJ 673, HD 157881, HIP 85295, SAO 122374, LHS 447, LTT 15175, PLX 3955.00, Wolf 718, MCC 794[6]
Database references
SIMBADdata

Gliese 673 is an orange dwarf star in the constellation Ophiuchus. It has a stellar classification of K7V.[2] Main sequence stars with this spectra have a mass in the range of 60–70% of solar mass (M☉) (comparable to the members of the binary star system 61 Cygni).

This star is relatively near the Sun at a distance of 25.2 light-years. In spite of this proximity, however, it is still too faint to be viewed by the unaided eye. It is considered a slowly rotating star with a relatively high proper motion.

Gliese 673 is among nearby K-type stars of a type in a 'sweet spot' between Sun-analog stars and M stars, in terms of the likelihood of life and its ease of detectability (in this case for planets in the system's outer conservative habitable zone), per analysis of Giada Arney from NASA's Goddard Space Flight Center.[7]

See also

References

  1. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  2. ^ a b c d e f Koen, C.; et al. (April 2010), "UBV(RI)C JHK observations of Hipparcos-selected nearby stars", Monthly Notices of the Royal Astronomical Society, 403 (4): 1949–1968, Bibcode:2010MNRAS.403.1949K, doi:10.1111/j.1365-2966.2009.16182.x
  3. ^ a b van Belle, Gerard T.; von Braun, Kaspar (April 2009), "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars", The Astrophysical Journal, 694 (2): 1085–1098, arXiv:0901.1206, Bibcode:2009ApJ...694.1085V, doi:10.1088/0004-637X/694/2/1085, S2CID 18370219
  4. ^ a b Frasca, A.; et al. (December 2009), "REM near-IR and optical photometric monitoring of pre-main sequence stars in Orion. Rotation periods and starspot parameters", Astronomy and Astrophysics, 508 (3): 1313–1330, arXiv:0911.0760, Bibcode:2009A&A...508.1313F, doi:10.1051/0004-6361/200913327, S2CID 118361131
  5. ^ a b Barnes, Sydney A. (November 2007), "Ages for Illustrative Field Stars Using Gyrochronology: Viability, Limitations, and Errors", The Astrophysical Journal, 669 (2): 1167–1189, arXiv:0704.3068, Bibcode:2007ApJ...669.1167B, doi:10.1086/519295, S2CID 14614725
  6. ^ "LHS 447 -- High proper-motion Star", SIMBAD, Centre de Données astronomiques de Strasbourg, archived from the original on 2023-03-28, retrieved 2011-10-15
  7. ^ Arney, Giada N. (2019). "The K Dwarf Advantage for Biosignatures on Directly Imaged Exoplanets". The Astrophysical Journal. 873 (1): L7. arXiv:2001.10458. Bibcode:2019ApJ...873L...7A. doi:10.3847/2041-8213/ab0651.


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