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58 Leonis

From Wikipedia, the free encyclopedia
Star in the constellation Leo
58 Leonis
Observation data
Epoch J2000      Equinox J2000
ConstellationLeo
Right ascension11h 00m 33.64811s[1]
Declination+03° 37′ 02.9766″[1]
Apparent magnitude (V)4.852[2]
Characteristics
Spectral typeK0.5 III Fe-0.5[3]
B−Vcolor index1.163[2]
Astrometry
Radial velocity (Rv)+5.98[2] km/s
Proper motion (μ)RA: +14.82[1]mas/yr
Dec.: −16.51[1]mas/yr
Parallax (π)9.05±0.20 mas[1]
Distance360 ± 8 ly
(110 ± 2 pc)
Absolute magnitude (MV)−1.04[4]
Details
Mass1.89[2] M
Luminosity182[2] L
Surface gravity (log g)1.8[4] cgs
Temperature4,519±52[2] K
Metallicity[Fe/H]−0.16±0.10[4] dex
Age1.69[2] Gyr
Other designations
58 Leo,BD+04°2407,FK5 1284,HD 95345,HIP 53807,HR 4291,SAO 118610,CCDM J11006+0337AB[5]
Database references
SIMBADdata

58 Leonis is a possiblebinary star[6] system in the southern part of the constellation ofLeo, near the border withSextans. It shines with anapparent magnitude of 4.85,[2] making it bright enough to be seen with the naked eye. An annualparallax shift of9.05±0.20 mas yields a distance estimate of 360 light years. It is moving further from the Sun with a heliocentricradial velocity of +6 km/s.[2]

This orange hued star is anevolvedK-typegiant with astellar classification ofK0.5 III Fe-0.5,[3] indicating a mild underabundance of iron in itsspectrum. It was identified as abarium star by P. M. Williams (1971).[7] These are theorized to be stars that show an enrichment ofs-process elements by mass transfer from a now-white dwarf companion when it passed through theasymptotic giant branch stage.[8] MacConnell et al. (1972) classified 58 Leonis as a marginal barium star.[4] De Castro et al. (2016) consider this to be only a probable barium star, because of the low degree ofs-process enrichment, and they rejected it from their sample. Rather than having an evolved companion, it may instead have formed from a cloud that was mildly enriched with s-process elements.[4]

References

[edit]
  1. ^abcdevan 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. ^abcdefghiLuck, R. Earle (2015), "Abundances in the Local Region. I. G and K Giants",Astronomical Journal,150 (3), 88,arXiv:1507.01466,Bibcode:2015AJ....150...88L,doi:10.1088/0004-6256/150/3/88,S2CID 118505114.
  3. ^abKeenan, 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,S2CID 123149047.
  4. ^abcdeDe Castro, D. B.; et al. (2016), "Chemical abundances and kinematics of barium stars",Monthly Notices of the Royal Astronomical Society,459 (4): 4299,arXiv:1604.03031,Bibcode:2016MNRAS.459.4299D,doi:10.1093/mnras/stw815
  5. ^"58 Leo".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2018-03-01.
  6. ^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.
  7. ^Williams, P. M. (February 1971), "Abundances in five newly-discovered BA II stars",The Observatory,91:37–39,Bibcode:1971Obs....91...37W.
  8. ^Bergeat, J.; Knapik, A. (May 1997), "The barium stars in the Hertzsprung-Russel diagram.",Astronomy and Astrophysics,321: L9,Bibcode:1997A&A...321L...9B.

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