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11 Leonis Minoris

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11 Leonis Minoris

A near-infrared (y band)light curvefor SV Leonis Minoris, adapted from Skiff and Lockwood (1986)[1]
Observation data
EpochJ2000EquinoxJ2000
Constellation Leo Minor
Right ascension 09h35m39.50219s[2]
Declination +35° 48′ 36.4770″[2]
Apparent magnitude(V) 5.54 + 14.0[3]
Characteristics
Spectral type G8V[4]+ M4[5]
U−Bcolor index 0.44/—
B−Vcolor index 0.77/—
Variable type RS CVn
Astrometry
Radial velocity(Rv)+14.40[6]km/s
Proper motion(μ)RA:−726.514mas/yr[2]
Dec.:−259.057mas/yr[2]
Parallax(π)89.0092 ± 0.0937mas[2]
Distance36.64 ± 0.04ly
(11.23 ± 0.01pc)
Absolute magnitude(MV)5.25±0.008[7]
Orbit[4]
Companion11 LMi B
Period(P)201yr
Semi-major axis(a)3.84″
Eccentricity(e)0.88
Inclination(i)117°
Details[8]
11 LMi A
Mass0.936±0.015M☉
Radius0.992±0.015R☉
Luminosity0.783±0.013L☉
Surface gravity(logg)4.44±0.02cgs
Temperature5,452±46K
Metallicity[Fe/H]0.34±0.02dex
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,GJ356,HD82885,HIP47080,HR3815,SAO61586,WDS09357+3549[12]
Database references
SIMBAD11 LMi A
11 LMi B
ARICNS11 LMi A
11 LMi B

11 Leonis Minorisis abinary star[3]located 36.64light yearsaway fromEarth,[2]in the northernconstellationofLeo Minor.[12]It is visible to the naked eye as a dim, yellow-hued star with anapparent visual magnitudeof 5.54.[3]The system is moving away from the Earth with a heliocentricradial velocityof +14.4 km/s.[6]It has a relatively highproper motion,traversing thecelestial sphereat the rate of 0.764arc secondsper annum.[13]

The primary component is aG-type main-sequence starwith astellar classificationof G8V,[4]which is slightly less massive and slightly dimmer than the Sun.[8]This is anRS Canum Venaticorum variablestar 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'smetallicity.[9]

There is a secondary component, a 14th[3]magnitude red dwarf star much dimmer than the primary. The pair have anorbital periodof 201 years with a higheccentricityof 0.88.[4]

References

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  1. ^abSkiff, 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
  2. ^abcdeVallenari, A.; et al. (Gaia collaboration) (2023)."GaiaData Release 3. Summary of the content and survey properties ".Astronomy and Astrophysics.674:A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID244398875. Gaia DR3 record for this sourceatVizieR.
  3. ^abcdEggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems",Monthly Notices of the Royal Astronomical Society,389(2): 869–879,arXiv:0806.2878,Bibcode:2008MNRAS.389..869E,doi:10.1111/j.1365-2966.2008.13596.x,S2CID14878976.
  4. ^abcdMalkov, 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
  5. ^Reid, I. Neill; Cruz, Kelle L.; Allen, Peter R.; Mungall, Finlay; Kilkenny, David; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R.; Lowrance, Patrick; Kirkpatrick, J. Davy; Burgasser, Adam J. (2004),"Meeting the Cool Neighbors. VIII. A Preliminary 20 Parsec Census from the NLTT Catalogue",The Astronomical Journal(Submitted manuscript),128(1): 463,arXiv:astro-ph/0404061,Bibcode:2004AJ....128..463R,doi:10.1086/421374,S2CID28314795
  6. ^abSoubiran, 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,S2CID16602121
  7. ^Park, Sunkyung; et al. (2013), "Wilson-Bappu Effect: Extended to Surface Gravity",The Astronomical Journal,146(4): 73,arXiv:1307.0592,Bibcode:2013AJ....146...73P,doi:10.1088/0004-6256/146/4/73,S2CID119187733.
  8. ^abSoubiran, C.; Creevey, O. L.; Lagarde, N.; Brouillet, N.; Jofré, P.; Casamiquela, L.; Heiter, U.; Aguilera-Gómez, C.; Vitali, S.; Worley, C.; de Brito Silva, D. (2024-02-01), "Gaia FGK benchmark stars: Fundamental Teff and log g of the third version",Astronomy and Astrophysics,682:A145,arXiv:2310.11302,Bibcode:2024A&A...682A.145S,doi:10.1051/0004-6361/202347136,ISSN0004-636111 Leonis Minoris' database entryatVizieR.
  9. ^abMaldonado, 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,S2CID119209183
  10. ^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,S2CID14911430.
  11. ^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,S2CID56066740,87.
  12. ^ab"* 11 LMi",SIMBAD,Centre de données astronomiques de Strasbourg,retrieved2015-06-02.
  13. ^Lépine, Sébastien; Shara, Michael M. (March 2005), "A Catalog of Northern Stars with Annual Proper Motions Larger than 0.15" (LSPM-NORTH Catalog) ",The Astronomical Journal,129(3): 1483–1522,arXiv:astro-ph/0412070,Bibcode:2005AJ....129.1483L,doi:10.1086/427854,S2CID2603568.
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