11 Leonis Minoris

From Wikipedia, the free encyclopedia
Jump to: navigation, search
11 Leonis Minoris A/B
Observation data
Epoch J2000      Equinox J2000
Constellation Leo Minor
Right ascension 09h 35m 39.50337s[1]
Declination +35° 48′ 36.4874″[1]
Apparent magnitude (V) 4.80/12.50[2]
Spectral type G8V[2] + M5V[citation needed]
U−B color index 0.44/—
B−V color index 0.77/—
Variable type RS CVn
Radial velocity (Rv) +14.40[3] km/s
Proper motion (μ) RA: -728.71[1] mas/yr
Dec.: -259.81[1] mas/yr
Parallax (π) 87.96 ± 0.32[1] mas
Distance 37.1 ± 0.1 ly
(11.37 ± 0.04 pc)
Companion 11 LMi B
Period (P) 201 yr
Semi-major axis (a) 3.84"
Eccentricity (e) 0.88
Inclination (i) 117°
11 LMi A
Mass 0.964[4] M
Radius 1.0029 ± 0.0158[4] R
Luminosity 0.7550 ± 0.0055[4] L
Temperature 5376 ± 43[4] K
Metallicity [Fe/H] +0.33[5] dex
Rotation 18.0 days[5]
Age 7.9[4] Gyr
11 LMi B
Mass 0.23[6] M
Other designations
11 Leonis Minoris, GJ 356, HD 82885, HIP 47080, HR 3815, SAO 61586, WDS 09357+3549[7]

11 Leonis Minoris (11 LMi) is a star system located 37 light years away from Earth, in the northern constellation of Leo Minor. The primary component is a G-type main sequence star of spectral type G8V, which is slightly more massive but slightly dimmer than Sol. This is an RS Canum Venaticorum variable star with its luminosity varying by 0.033 magnitudes over a period of 18 days.[8] Compared to the Sun, it has more than double the abundance of elements more massive than helium—what astronomers term the star's metallicity.[5]

There is a secondary component, a red dwarf star much dimmer than the primary. It has a highly eccentric orbit ranging from roughly 4 AU to 63 AU from the primary.[citation needed]

Popular culture[edit]

John J. Lumpkin used the star system in his novel Through Struggle, the Stars.


  1. ^ a b c d e van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357 
  2. ^ a b c Malkov, O. Yu.; et al. (2012), "Dynamical masses of a selected sample of orbital binaries", Astronomy & Astrophysics 546: 5, Bibcode:2012A&A...546A..69M, doi:10.1051/0004-6361/201219774, A69 
  3. ^ Soubiran, C.; et al. (2008), "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants", Astronomy and Astrophysics 480 (1): 91–101, arXiv:0712.1370, Bibcode:2008A&A...480...91S, doi:10.1051/0004-6361:20078788 
  4. ^ a b c d e Boyajian, Tabetha S.; et al. (July 2013), "Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations", The Astrophysical Journal 771 (1): 40, arXiv:1306.2974, Bibcode:2013ApJ...771...40B, doi:10.1088/0004-637X/771/1/40. 
  5. ^ a b c Maldonado, J.; et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics 521: A12, arXiv:1007.1132, Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948 
  6. ^ Tokovinin, Andrei (April 2014), "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs", The Astronomical Journal 147 (4): 14, arXiv:1401.6827, Bibcode:2014AJ....147...87T, doi:10.1088/0004-6256/147/4/87, 87. 
  7. ^ "11 LMi -- Variable of RS CVn type", SIMBAD Astronomical Database (Centre de Données astronomiques de Strasbourg), retrieved 2015-06-02. 
  8. ^ Skiff, B. A.; et al. (March 1986), "The photometric variability of solar-type stars. V - The standard stars 10 and 11 Leonis Minoris", Publications of the Astronomical Society of the Pacific 98: 338–341, Bibcode:1986PASP...98..338S, doi:10.1086/131763 

External links[edit]