11 Leonis Minoris

11 Leonis Minoris is a binary star^[3] located 36.64 light years away from Earth,^[2] in the northern constellation of Leo Minor.^[12] It is visible to the naked eye as a dim, yellow-hued star with an apparent visual magnitude of 5.54.^[3] The system is moving away from the Earth with a heliocentric radial velocity of +14.4 km/s.^[6] It has a relatively high proper motion, traversing the celestial sphere at the rate of 0.764 arc seconds per annum.^[13]

11 Leonis Minoris

A near-infrared (y band) light curve for SV Leonis Minoris, adapted from Skiff and Lockwood (1986)[1]
Observation data Epoch J2000      Equinox J2000
Constellation	Leo Minor
Right ascension	09h 35m 39.50219s[2]
Declination	+35° 48′ 36.4770″[2]
Apparent magnitude (V)	5.54 + 14.0[3]
Characteristics
Spectral type	G8V[4] + M4[5]
U−B color index	0.44/—
B−V color index	0.77/—
Variable type	RS CVn
Astrometry
Radial velocity (Rv)	+14.40[6] km/s
Proper motion (μ)	RA: −726.514 mas/yr[2] Dec.: −259.057 mas/yr[2]
Parallax (π)	89.0092±0.0937 mas[2]
Distance	36.64 ± 0.04 ly (11.23 ± 0.01 pc)
Absolute magnitude (MV)	5.25±0.008[7]
Orbit[4]
Companion	11 LMi B
Period (P)	201 yr
Semi-major axis (a)	3.84″
Eccentricity (e)	0.88
Inclination (i)	117°
Details[8]
11 LMi A
Mass	0.936±0.015 M☉
Radius	0.992±0.015 R☉
Luminosity	0.783±0.013 L☉
Surface gravity (log g)	4.44±0.02 cgs
Temperature	5,452±46 K
Metallicity [Fe/H]	0.34±0.02 dex
Rotation	18.0 days[9]
Age	7.9[10] Gyr
11 LMi B
Mass	0.23[11] M☉
Other designations
11 LMi, SV Leonis Minoris, BD+36°1979, GJ 356, HD 82885, HIP 47080, HR 3815, SAO 61586, WDS 09357+3549[12]
Database references
SIMBAD	11 LMi A
	11 LMi B
ARICNS	11 LMi A
	11 LMi B

The primary component is a G-type main-sequence star with a stellar classification of G8V,^[4] which is slightly less massive and slightly dimmer than the Sun.^[8] This is an RS Canum Venaticorum variable star with its luminosity varying by 0.033 magnitudes over a period of 18 days.^[1] Compared to the Sun, it has more than double the abundance of elements more massive than helium—what astronomers term the star's metallicity.^[9]

There is a secondary component, a 14th^[3] magnitude red dwarf star much dimmer than the primary. The pair have an orbital period of 201 years with a high eccentricity of 0.88.^[4]