Astronomy:11 Leonis Minoris
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Short description: Star in the constellation Leo Minor
 A near-infrared (y band) light curve for SV Leonis Minoris, adapted from Skiff and Lockwood (1986)[1] | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Leo Minor |
| Right ascension | 09h 35m 39.50181s[2] |
| Declination | +35° 48′ 36.4841″[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: −726.201[2] mas/yr Dec.: −259.506[2] mas/yr |
| Parallax (π) | 89.2581 ± 0.1928[2] mas |
| Distance | 36.54 ± 0.08 ly (11.20 ± 0.02 pc) |
| Absolute magnitude (MV) | 5.25±0.008[7] |
| Orbit[4] | |
| 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[8] M☉ |
| Radius | 1.0029±0.0158[8] R☉ |
| Luminosity | 0.7550±0.0055[8] L☉ |
| Temperature | 5376±43[8] K |
| Metallicity [Fe/H] | +0.33[9] dex |
| Rotation | 18.0 days[9] |
| Age | 7.9[8] Gyr |
| 11 LMi B | |
| Mass | 0.23[10] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | 11 LMi A |
| 11 LMi B | |
| ARICNS | 11 LMi A |
| 11 LMi B | |
11 Leonis Minoris is a binary star[3] located 36.5 light years away from Earth,[2] in the northern constellation of Leo Minor.[11] 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.[12]
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]
References
- ↑ 1.0 1.1 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, doi:10.1086/131763, Bibcode: 1986PASP...98..338S
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 Eggleton, 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ 4.0 4.1 4.2 4.3 Malkov, O. Yu. et al. (2012), "Dynamical masses of a selected sample of orbital binaries", Astronomy & Astrophysics 546: 5, doi:10.1051/0004-6361/201219774, A69, Bibcode: 2012A&A...546A..69M
- ↑ Reid, I. Neill; Cruz, Kelle L.; Allen, Peter R.; Mungall, Finlay; Kilkenny, David; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J. et al. (2004), "Meeting the Cool Neighbors. VIII. A Preliminary 20 Parsec Census from the NLTT Catalogue", The Astronomical Journal 128 (1): 463, doi:10.1086/421374, Bibcode: 2004AJ....128..463R, https://cds.cern.ch/record/728686
- ↑ 6.0 6.1 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, doi:10.1051/0004-6361:20078788, Bibcode: 2008A&A...480...91S
- ↑ Park, Sunkyung et al. (2013), "Wilson-Bappu Effect: Extended to Surface Gravity", The Astronomical Journal 146 (4): 73, doi:10.1088/0004-6256/146/4/73, Bibcode: 2013AJ....146...73P.
- ↑ 8.0 8.1 8.2 8.3 8.4 8.5 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, doi:10.1088/0004-637X/771/1/40, Bibcode: 2013ApJ...771...40B.
- ↑ 9.0 9.1 9.2 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, doi:10.1051/0004-6361/201014948, Bibcode: 2010A&A...521A..12M
- ↑ Tokovinin, Andrei (April 2014), "From Binaries to Multiples. II. Hierarchical Multiplicity of F and G Dwarfs", The Astronomical Journal 147 (4): 14, doi:10.1088/0004-6256/147/4/87, 87, Bibcode: 2014AJ....147...87T.
- ↑ 11.0 11.1 "* 11 LMi". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+11+LMi.
- ↑ 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, doi:10.1086/427854, Bibcode: 2005AJ....129.1483L.
External links
- "Binary Catalog". Archived from the original on September 28, 2007. https://archive.today/20070928095822/http://159.226.168.243/astrodata/ds2006/ORB6/CATHTML/orb6orbits.html. Retrieved April 4, 2007.
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