11 Leonis Minoris

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]
Distance36.64 ± 0.04 ly
(11.23 ± 0.01 pc)
Absolute magnitude (MV)5.25±0.008[7]
Orbit[4]
Companion11 LMi B
Period (P)201 yr
Semi-major axis (a)3.84″
Eccentricity (e)0.88
Inclination (i)117°
Details[8]
11 LMi A
Mass0.936±0.015 M☉
Radius0.992±0.015 R☉
Luminosity0.783±0.013 L☉
Surface gravity (log g)4.44±0.02 cgs
Temperature5,452±46 K
Metallicity [Fe/H]0.34±0.02 dex
Rotation18.0 days[9]
Age7.9[10] Gyr
11 LMi B
Mass0.23[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
SIMBAD11 LMi A
11 LMi B
ARICNS11 LMi A
11 LMi B

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]

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]

  1. ^ a b Cite error: The named reference pasp98_338 was invoked but never defined (see the help page).
  2. ^ a b c d e Cite error: The named reference DR3 was invoked but never defined (see the help page).
  3. ^ a b c d Cite error: The named reference Eggleton2008 was invoked but never defined (see the help page).
  4. ^ a b c d Cite error: The named reference aa546_A69 was invoked but never defined (see the help page).
  5. ^ Cite error: The named reference Reid2004 was invoked but never defined (see the help page).
  6. ^ a b Cite error: The named reference aaa480 was invoked but never defined (see the help page).
  7. ^ Cite error: The named reference park2013 was invoked but never defined (see the help page).
  8. ^ a b Cite error: The named reference Soubiran2024 was invoked but never defined (see the help page).
  9. ^ a b Cite error: The named reference aaa521_A12 was invoked but never defined (see the help page).
  10. ^ Cite error: The named reference Boyajian2013 was invoked but never defined (see the help page).
  11. ^ Cite error: The named reference aj147_4_87 was invoked but never defined (see the help page).
  12. ^ a b Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  13. ^ Cite error: The named reference Lepine2005 was invoked but never defined (see the help page).