11 Leonis Minoris

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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]
Characteristics
Spectral type G8V[2] + M5V[citation needed]
U−B color index 0.44/—
B−V color index 0.77/—
Variable type RS CVn
Astrometry
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)
Absolute magnitude (MV) 5.25±0.008[4]
Orbit[2]
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[5] M
Radius 1.0029 ± 0.0158[5] R
Luminosity 0.7550 ± 0.0055[5] L
Temperature 5376 ± 43[5] K
Metallicity [Fe/H] +0.33[6] dex
Rotation 18.0 days[6]
Age 7.9[5] Gyr
11 LMi B
Mass 0.23[7] M
Other designations
11 Leonis Minoris, GJ 356, HD 82885, HIP 47080, HR 3815, SAO 61586, WDS 09357+3549[8]

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.[9] Compared to the Sun, it has more than double the abundance of elements more massive than helium—what astronomers term the star's metallicity.[6]

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.[citation needed]

References[edit]

  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:0708.1752Freely accessible, 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:0712.1370Freely accessible, Bibcode:2008A&A...480...91S, doi:10.1051/0004-6361:20078788 
  4. ^ Park, Sunkyung; et al. (2013), "Wilson-Bappu Effect: Extended to Surface Gravity", The Astronomical Journal, 146 (4): 73, arXiv:1307.0592Freely accessible, Bibcode:2013AJ....146...73P, doi:10.1088/0004-6256/146/4/73. 
  5. ^ 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:1306.2974Freely accessible, Bibcode:2013ApJ...771...40B, doi:10.1088/0004-637X/771/1/40. 
  6. ^ 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:1007.1132Freely accessible, Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948 
  7. ^ Tokovinin, Andrei (April 2014), "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs", The Astronomical Journal, 147 (4): 14, arXiv:1401.6827Freely accessible, Bibcode:2014AJ....147...87T, doi:10.1088/0004-6256/147/4/87, 87. 
  8. ^ "11 LMi -- Variable of RS CVn type", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2015-06-02. 
  9. ^ 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]