11 Leonis Minoris
Star in the constellation Leo Minor
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11 Leonis Minoris is a binary star[2] located 36.64 light years away from Earth,[1] 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.[2] 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]
  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Leo Minor |
| Right ascension | 09h 35m 39.50219s[1] |
| Declination | +35° 48â² 36.4770â³[1] |
| Apparent magnitude (V) | 5.54 + 14.0[2] |
| Characteristics | |
| Evolutionary stage | main sequence[1] |
| Spectral type | G8V[3] + M4[4] |
| Variable type | RS CVn[5] |
| Astrometry | |
| Radial velocity (Rv) | +14.40[6] km/s |
| Proper motion (μ) | RA: â726.514 mas/yr[1] Dec.: â259.057 mas/yr[1] |
| Parallax (Ï) | 89.0092±0.0937 mas[1] |
| Distance | 36.64 ± 0.04 ly (11.23 ± 0.01 pc) |
| Absolute magnitude (MV) | 5.25±0.008[7] |
| Orbit[3] | |
| Name | 11 LMi B |
| Period (P) | 201 yr |
| Semi-major axis (a) | 3.84â³ |
| Eccentricity (e) | 0.88 |
| Inclination (i) | 117° |
| Details[8] | |
| 11 LMi A | |
| Mass | 0.936±0.015 Mâ |
| Radius | 0.992±0.015 Râ |
| Luminosity | 0.783±0.013 Lâ |
| 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] Mâ |
| 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,[3] 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.[5] Compared to the Sun, it has more than double the abundance of elements more massive than heliumâwhat astronomers term the star's metallicity.[9]
There is a secondary component, a 14th[2] 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.[3]