11 Leonis Minoris is a binary star[3] located 36.5 light years away from Earth,[2] in the northern constellation of Leo Minor.[11] 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.[12]
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 39.50181s[2] |
Declination | +35° 48′ 36.4841″[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: −726.201[2] mas/yr Dec.: −259.506[2] mas/yr |
Parallax (π) | 89.2581 ± 0.1928 mas[2] |
Distance | 36.54 ± 0.08 ly (11.20 ± 0.02 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 | |
11 LMi A | |
Mass | 0.964[8] M☉ |
Radius | 1.0029±0.0158[8] R☉ |
Luminosity | 0.7550±0.0055[8] L☉ |
Temperature | 5376±43[8] K |
Metallicity [Fe/H] | +0.33[9] dex |
Rotation | 18.0 days[9] |
Age | 7.9[8] Gyr |
11 LMi B | |
Mass | 0.23[10] M☉ |
Other designations | |
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]