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15 Leonis Minoris
	Location of 15 Leo Minoris (circled)
Observation data; Epoch J2000.0 Equinox J2000.0
Constellation	Ursa Major
Right ascension	09h 48m 35.37130s
Declination	+46° 01′ 15.6338″
Apparent magnitude (V)	5.08
Characteristics
Spectral type	G0 IV-V
U−B color index	+0.175
B−V color index	0.619±0.007
Astrometry
Radial velocity (Rv)	5.20±0.09 km/s
Proper motion (μ)	RA: 221.788 mas/yr ; Dec.: −92.816 mas/yr
Parallax (π)	52.8994 ± 0.1260 mas
Distance	61.7 ± 0.1 ly ; (18.90 ± 0.05 pc)
Absolute magnitude (MV)	3.75
Details
Mass	1.15 M☉
Radius	1.52 R☉
Luminosity	2.912±0.010 L☉
Surface gravity (log g)	4.04 cgs
Temperature	5,859 K
Metallicity [Fe/H]	0.01 dex
Rotational velocity (v sin i)	3.97 km/s
Age	9.3 Gyr
Other designations
	15 LMi, BD+46°1551, FK5 1255, GJ 368, HD 84737, HIP 48113, HR 3881, SAO 43046
Database references
SIMBAD	data

15 Leonis Minoris is the Flamsteed designation for a single^[13] star in the northern circumpolar constellation of Ursa Major. It has an apparent visual magnitude of 5.08,^[3] making it a fifth magnitude star that is visible to the naked eye. Based on parallax measurements, it is located at a distance of 61.7 light years from the Sun. The star has been examined for an infrared excess, but none was detected.^[14]

This star has a stellar classification of G0 IV-V^[4] with an age of about 9.3 billion years,^[11] which suggests that it is an older G-type main sequence star that may be evolving into a subgiant as the hydrogen at its core runs out. The estimated mass of the star is 15% greater than the Sun's mass,^[8] and it is larger in girth than the Sun by +52%.^[9] It is spinning with a projected rotational velocity of 4 km/s.^[10] The star is radiating almost three^[2] times the luminosity of the Sun from its photosphere at an effective temperature of 5,859 K,^[4] giving it the yellow-hued glow of a G-type star.^[15]

References

^ Hoffleit, D. (1979), "Discordances in Star Designations", Bulletin d'Information du Centre de Données Stellaires, 17: 38, Bibcode:1979BICDS..17...38H.
^ ^a ^b ^c ^d ^e ^f ^g Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
^ ^a ^b ^c Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
^ ^a ^b ^c ^d ^e ^f Gray, R. O.; et al. (July 2006), "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
^ Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", SIMBAD Astronomical Database, Bibcode:1986EgUBV........0M.
^ Nidever, David L.; et al. (August 2002), "Radial Velocities for 889 Late-Type Stars", The Astrophysical Journal Supplement Series, 141 (2): 503–522, arXiv:astro-ph/0112477, Bibcode:2002ApJS..141..503N, doi:10.1086/340570, S2CID 51814894.
^ Luck, R. Earle; Heiter, Ulrike (2006), "Dwarfs in the Local Region", The Astronomical Journal, 131 (6): 3069–3092, Bibcode:2006AJ....131.3069L, doi:10.1086/504080.
^ ^a ^b Ramírez, I.; et al. (September 2012), "Lithium Abundances in nearby FGK Dwarf and Subgiant Stars: Internal Destruction, Galactic Chemical Evolution, and Exoplanets", The Astrophysical Journal, 756 (1): 46, arXiv:1207.0499, Bibcode:2012ApJ...756...46R, doi:10.1088/0004-637X/756/1/46, S2CID 119199829.
^ ^a ^b Takeda, Genya; Ford, Eric B.; Sills, Alison; Rasio, Frederic A.; Fischer, Debra A.; Valenti, Jeff A. (2007), "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog", The Astrophysical Journal Supplement Series, 168 (2): 297, arXiv:astro-ph/0607235, Bibcode:2007ApJS..168..297T, doi:10.1086/509763, S2CID 18775378.
^ ^a ^b Martínez-Arnáiz, R.; et al. (September 2010), "Chromospheric activity and rotation of FGK stars in the solar vicinity. An estimation of the radial velocity jitter" (PDF), Astronomy and Astrophysics, 520: A79, arXiv:1002.4391, Bibcode:2010A&A...520A..79M, doi:10.1051/0004-6361/200913725, S2CID 43455849, archived from the original (PDF) on 2017-09-22, retrieved 2018-11-04.
^ ^a ^b Ballering, Nicholas P.; et al. (September 2013), "A Trend between Cold Debris Disk Temperature and Stellar Type: Implications for the Formation and Evolution of Wide-orbit Planets", The Astrophysical Journal, 775 (1): 14, arXiv:1308.2223, Bibcode:2013ApJ...775...55B, doi:10.1088/0004-637X/775/1/55, S2CID 119113700, 55.
^ "* 15 LMi", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2016-07-19.
^ 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.
^ Moro-Martín, A.; et al. (March 2015), "Does the Presence of Planets Affect the Frequency and Properties of Extrasolar Kuiper Belts? Results from the Herschel Debris and Dunes Surveys", The Astrophysical Journal, 801 (2): 28, arXiv:1501.03813, Bibcode:2015ApJ...801..143M, doi:10.1088/0004-637X/801/2/143, S2CID 55170390, 143.
^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2016-07-25.