Astronomy:20 Leonis Minoris
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Short description: Star in the constellation Leo Minor
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Leo Minor |
| Right ascension | 10h 01m 00.65765s[1] |
| Declination | +31° 55′ 25.2151″[1] |
| Apparent magnitude (V) | +5.40[2] |
| Characteristics | |
| Spectral type | G3 Va Hδ1[3] + M7 V[4] |
| U−B color index | +0.27[5] |
| B−V color index | +0.65[5] |
| Astrometry | |
| Radial velocity (Rv) | +55.96±0.09[6] km/s |
| Proper motion (μ) | RA: −527.63±0.30[1] mas/yr Dec.: −429.42±0.18[1] mas/yr |
| Parallax (π) | 66.46 ± 0.32[1] mas |
| Distance | 49.1 ± 0.2 ly (15.05 ± 0.07 pc) |
| Absolute magnitude (MV) | 4.46[7] |
| Details | |
| 20 LMi A | |
| Mass | 1.12[8] M☉ |
| Radius | 1.247±0.021[9] R☉ |
| Luminosity | 1.378±0.027[9] L☉ |
| Temperature | 5,735±5.6[10] K |
| Rotation | 10.64±0.14 d[2] |
| Age | 6.2–7.7[11] Gyr |
| 20 LMi B | |
| Mass | 0.11[8] M☉ |
| Rotation | 19.2687 d[4] |
| Other designations | |
| Database references | |
| SIMBAD | data |
20 Leonis Minoris is a binary star system in the northern constellation of Leo Minor. It is faintly visible to the naked eye, having an apparent visual magnitude of +5.4.[2] Based upon an annual parallax shift of 66.46 mas, it is located 49 light years from the Sun. The star has a relatively high proper motion[3] and is moving away from the Sun with a radial velocity of +56 km/s.[6] The system made its closest approach about 150,000 years ago when it came within 32.2 ly (9.86 pc).[13]
The primary member of this system is a G-type main-sequence star with a stellar classification of G3 Va Hδ1.[3] It has 12% more mass and a 25% larger radius than the Sun. The star is about seven[11] billion years old and is spinning with a rotation period of 10.6 days.[2] The small companion is an active red dwarf star that has a relatively high metallicity.[14] The two stars are currently separated by 14.5 arc seconds, corresponding to a projected separation of 2016 AU.[8]
In 2020, a candidate exoplanet was detected orbiting 20 Leonis Minoris (HD 86728). With a minimum mass of 0.032 |♃|J}}}}}} (10.2 M⊕) and an orbital period of 31 days, this would most likely be a hot Neptune.[15]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (unconfirmed) | ≥0.032+0.005 −0.005 MJ |
0.2003+0.00007 −0.00007 |
31.15+0.02 −0.02 |
0.2+0.2 −0.1 |
— | — |
References
- ↑ 1.0 1.1 1.2 1.3 1.4 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V, http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=I/311/hip2&recno=48928, retrieved 2009-12-18.
- ↑ 2.0 2.1 2.2 2.3 Hempelmann, A. et al. (February 2016), "Measuring rotation periods of solar-like stars using TIGRE. A study of periodic CaII H+K S-index variability", Astronomy & Astrophysics 586: 19, doi:10.1051/0004-6361/201526972, A14, Bibcode: 2016A&A...586A..14H.
- ↑ 3.0 3.1 3.2 Keenan, P.; McNeil, R. (October 1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series 71: 245–266, doi:10.1086/191373, Bibcode: 1989ApJS...71..245K.
- ↑ 4.0 4.1 West, Andrew A. et al. (October 2015), "An Activity-Rotation Relationship and Kinematic Analysis of Nearby Mid-to-Late-Type M Dwarfs", The Astrophysical Journal 812 (1): 12, doi:10.1088/0004-637X/812/1/3, 3, Bibcode: 2015ApJ...812....3W.
- ↑ 5.0 5.1 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode: 1986EgUBV........0M.
- ↑ 6.0 6.1 Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters 32 (11): 759–771. doi:10.1134/S1063773706110065. Bibcode: 2006AstL...32..759G.
- ↑ Holmberg, J. et al. (July 2009), "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics", Astronomy and Astrophysics 501 (3): 941–947, doi:10.1051/0004-6361/200811191, Bibcode: 2009A&A...501..941H.
- ↑ 8.0 8.1 8.2 Tokovinin, A.; Kiyaeva, O. (February 2016), "Eccentricity distribution of wide binaries", Monthly Notices of the Royal Astronomical Society 456 (2): 2070−2079, doi:10.1093/mnras/stv2825, Bibcode: 2016MNRAS.456.2070T.
- ↑ 9.0 9.1 Boyajian, Tabetha S. et al. (February 2012), "Stellar Diameters and Temperatures. I. Main-sequence A, F, and G Stars", The Astrophysical Journal 746 (1): 101, doi:10.1088/0004-637X/746/1/101, Bibcode: 2012ApJ...746..101B. See Table 10.
- ↑ Kovtyukh; Soubiran, C.; Belik, S. I.; Gorlova, N. I. (2003), "High precision effective temperatures for 181 F-K dwarfs from line-depth ratios", Astronomy and Astrophysics 411 (3): 559–564, doi:10.1051/0004-6361:20031378, Bibcode: 2003A&A...411..559K
- ↑ 11.0 11.1 Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal 687 (2): 1264–1293, doi:10.1086/591785, Bibcode: 2008ApJ...687.1264M
- ↑ "HD 86728". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+86728.
- ↑ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics 575: 13, doi:10.1051/0004-6361/201425221, A35, Bibcode: 2015A&A...575A..35B.
- ↑ Gizis, J. E. et al. (2000), "Two Nearby M Dwarf Binaries from 2MASS", Monthly Notices of the Royal Astronomical Society 311 (2): 385, doi:10.1046/j.1365-8711.2000.03060.x, Bibcode: 2000MNRAS.311..385G
- ↑ 15.0 15.1 Hirsch, Lea A. et al. (2021), "Understanding the Impacts of Stellar Companions on Planet Formation and Evolution: A Survey of Stellar and Planetary Companions within 25 pc", The Astronomical Journal 161 (3): 134, doi:10.3847/1538-3881/abd639, Bibcode: 2021AJ....161..134H.
External links
- "4C00774". ARICNS. http://www.ari.uni-heidelberg.de/datenbanken/aricns/cnspages/4c00774.htm. Retrieved 2006-07-31.
See also
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