58 Leonis is a possible binary star[6] system in the southern part of the constellation of Leo, near the border with Sextans. It shines with an apparent magnitude of 4.85,[2] making it bright enough to be seen with the naked eye. An annual parallax shift of 9.05±0.20 mas yields a distance estimate of 360 light years. It is moving further from the Sun with a heliocentric radial velocity of +6 km/s.[2]
This orange hued star is an evolved K-type giant with a stellar classification of K0.5 III Fe-0.5,[3] indicating a mild underabundance of iron in its spectrum. It was identified as a barium star by P. M. Williams (1971).[7] These are theorized to be stars that show an enrichment of s-process elements by mass transfer from a now-white dwarf companion when it passed through the asymptotic 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 of s-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]
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