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Chi Leonis

In the current context, Chi Leonis has become a relevant topic of great interest to society. Over time, Chi Leonis has gained importance and has generated a great impact in different areas, from politics to technology. That is why it is crucial to fully explore all the dimensions and repercussions that Chi Leonis has in our modern world. In this article, we will delve into the analysis and study of Chi Leonis, addressing its origins, evolution and its influence in different sectors. Furthermore, we will reflect on the future implications that Chi Leonis could have on society and how these can best be addressed.

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χ Leonis
Location of χ Leonis (circled in red)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Leo
Right ascension 11h 05m 01.02754s[1]
Declination +07° 20′ 09.6235″[1]
Apparent magnitude (V) 4.63[2]
Characteristics
Evolutionary stage Main sequence[3]
Spectral type F2III-IVv[4]
U−B color index +0.06[2]
B−V color index +0.33[2]
Astrometry
Radial velocity (Rv)+4.7[5] km/s
Proper motion (μ) RA: −344.28[1] mas/yr
Dec.: −47.65[1] mas/yr
Parallax (π)34.49±0.20 mas[1]
Distance94.6 ± 0.5 ly
(29.0 ± 0.2 pc)
Absolute magnitude (MV)+2.31[6]
Details
Mass1.62[7] M☉
Radius1.99[8] R☉
Luminosity9.9[6] L☉
Surface gravity (log g)4.02[7] cgs
Temperature7022±80[7] K
Metallicity +0.03[7] dex
Rotational velocity (v sin i)25±1[4] km/s
Age1.40[7] Gyr
Other designations
χ Leo, 63 Leo, BD+08°2455, FK5 418, HD 96097, HIP 54182, HR 4310, SAO 118648[9]
Database references
SIMBADdata

Chi Leonis, Latinized from χ Leonis, is a double star in the constellation Leo. It is visible to the naked eye with an apparent visual magnitude of 4.63.[2] The distance to this star, as determined using parallax measurements,[1] is around 95 light years. It has an annual proper motion of 346 mas.[10]

This is most likely a binary star system.[11] The primary component has a stellar classification of F2III-IVv, which at first would classify it as a F-type star between the giant and subgiant evolutionary stages,[4] but evolutionary models suggest the star is instead in the main sequence.[3][12] It has an estimated 162% of the Sun's mass[7] and nearly twice the Sun's radius.[8] The companion is a magnitude 11.0 star at an angular separation of 4.1″ along a position angle of 264°, as of 1990.[13]

Observation

On 18 October 2015, it was occulted by Mars as viewed from East Asia and Japan.[14]: 165 

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 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.
  4. ^ a b c Royer, F.; et al. (October 2002), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy and Astrophysics, 393: 897–911, arXiv:astro-ph/0205255, Bibcode:2002A&A...393..897R, doi:10.1051/0004-6361:20020943, S2CID 14070763.
  5. ^ Wilson, R. E. (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Carnegie Institute of Washington, D.C., Bibcode:1953GCRV..C......0W.
  6. ^ 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.
  7. ^ a b c d e f Casagrande, L.; et al. (2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy & Astrophysics, 530 (A138): 21, arXiv:1103.4651, Bibcode:2011A&A...530A.138C, doi:10.1051/0004-6361/201016276, S2CID 56118016.
  8. ^ a b Rachford, Brian L.; Foight, Dillon R. (June 2009), "Chromospheric Variability in Early F-Type Stars", The Astrophysical Journal, 698 (1): 786–802, arXiv:0904.1620, Bibcode:2009ApJ...698..786R, doi:10.1088/0004-637X/698/1/786, S2CID 693296.
  9. ^ "* chi Leo". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-09-29.{{cite web}}: CS1 maint: postscript (link)
  10. ^ Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog)", The Astronomical Journal, 129 (3): 1483–1522, arXiv:astro-ph/0412070, Bibcode:2005AJ....129.1483L, doi:10.1086/427854, S2CID 2603568.
  11. ^ 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.
  12. ^ "20.2.1 astrophysical_parameters‣ 20.2 Astrophysical parameter tables ‣ Chapter 20 Datamodel description ‣ Part V Gaia archive ‣ Gaia Data Release 3 Documentation release 1.3". gea.esac.esa.int. Retrieved 2025-06-01.
  13. ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466–3471, Bibcode:2001AJ....122.3466M, doi:10.1086/323920.
  14. ^ Meeus, Jan (2002). "Mutual occultations of planets". More Mathematical Astronomy Morsels (PDF). pp. 174–185. ISBN 0943396743.
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