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]
 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] |
| Distance | 36.64 ± 0.04 ly (11.23 ± 0.01 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[8] | |
| 11 LMi A | |
| Mass | 0.936±0.015 M☉ |
| Radius | 0.992±0.015 R☉ |
| Luminosity | 0.783±0.013 L☉ |
| Surface gravity (log g) | 4.44±0.02 cgs |
| Temperature | 5,452±46 K |
| Metallicity [Fe/H] | 0.34±0.02 dex |
| Rotation | 18.0 days[9] |
| Age | 7.9[10] Gyr |
| 11 LMi B | |
| Mass | 0.23[11] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | 11 LMi A |
| 11 LMi B | |
| ARICNS | 11 LMi A |
| 11 LMi B | |
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
edit- ^ a b 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
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data 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. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
- ^ a b c d 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
- ^ 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, S2CID 28314795
- ^ a b 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, S2CID 16602121
- ^ 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, S2CID 119187733.
- ^ a b Soubiran, 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, ISSN 0004-6361 11 Leonis Minoris' database entry at VizieR.
- ^ a b 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, S2CID 119209183
- ^ 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, S2CID 14911430.
- ^ 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, S2CID 56066740, 87.
- ^ a b "* 11 LMi", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2015-06-02.
- ^ 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, S2CID 2603568.
External links
edit- "Binary Catalog", archived from the original on September 28, 2007, retrieved April 4, 2007