58 Leonis is a possible binary star system in the southern part of the constellation of Leo, near the border with Sextans. It shines with an apparent magnitude of 4.85, making it bright enough to be seen with the naked eye. An annual parallax shift of yields a distance estimate of 360 light years. It is moving further from the Sun with a heliocentric radial velocity of +6 km/s.
This orange hued star is an evolved K-type giant with a stellar classification of, indicating a mild underabundance of iron in its spectrum. It was identified as a barium star by P. M. Williams (1971). 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. MacConnell et al. (1972) classified 58 Leonis as a marginal barium star. 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.