58 Leonis
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Leo |
| Right ascension | 11h 00m 33.64811s |
| Declination | +03° 37′ 02.9766″ |
| Apparent magnitude (V) | 4.852 |
| Characteristics | |
| Spectral type | K0.5 III Fe-0.5 |
| B−V color index | 1.163 |
| Astrometry | |
| Radial velocity (Rv) | +5.98 km/s |
| Proper motion (μ) | RA: +14.82 mas/yr Dec.: −16.51 mas/yr |
| Parallax (π) | 9.05±0.20 mas |
| Distance | 360 ± 8 ly (110 ± 2 pc) |
| Absolute magnitude (MV) | −1.04 |
| Details | |
| Mass | 1.89 M☉ |
| Luminosity | 182 L☉ |
| Surface gravity (log g) | 1.8 cgs |
| Temperature | 4,519±52 K |
| Metallicity [Fe/H] | −0.16±0.10 dex |
| Age | 1.69 Gyr |
| Other designations | |
| 58 Leo, BD+04°2407, FK5 1284, HD 95345, HIP 53807, HR 4291, SAO 118610, CCDM J11006+0337AB | |
| Database references | |
| SIMBAD | data |
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 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.
This orange hued star is an evolved K-type giant with a stellar classification of K0.5 III Fe-0.5, 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.