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15 Leonis Minoris

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Star in the constellation Ursa Major
15 Leonis Minoris
Location of 15 Leo Minoris (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
ConstellationUrsa Major[1]
Right ascension09h 48m 35.37130s[2]
Declination+46° 01′ 15.6338″[2]
Apparent magnitude (V)5.08[3]
Characteristics
Spectral typeG0 IV-V[4]
U−Bcolor index+0.175[5]
B−Vcolor index0.619±0.007[3]
Astrometry
Radial velocity (Rv)5.20±0.09[6] km/s
Proper motion (μ)RA: 221.788[2]mas/yr
Dec.: −92.816[2]mas/yr
Parallax (π)52.8994±0.1260 mas[2]
Distance61.7 ± 0.1 ly
(18.90 ± 0.05 pc)
Absolute magnitude (MV)3.75[7]
Details
Mass1.15[8] M
Radius1.52[9] R
Luminosity2.912±0.010[2] L
Habitable zone inner limit1.25[10]AU
Habitable zone outer limit2.93[10] AU
Surface gravity (log g)4.04[4] cgs
Temperature5,859[4] K
Metallicity[Fe/H]0.01[4] dex
Rotational velocity (v sin i)3.97[11] km/s
Age9.3[12] Gyr
Other designations
15 LMi,BD+46°1551,FK5 1255,GJ 368,HD 84737,HIP 48113,HR 3881,SAO 43046[13]
Database references
SIMBADdata

15 Leonis Minoris is theFlamsteed designation for a single[14]star in the northerncircumpolar constellation ofUrsa Major. It has anapparent visual magnitude of 5.08,[3] making it a fifth magnitude star that is visible to the naked eye. Based onparallax measurements, it is located at a distance of 61.7 light years from theSun. The star has been examined for aninfrared excess, but none was detected.[15]

This star has astellar classification of G0 IV-V[4] with an age of about 9.3 billion years,[12] which suggests that it is an olderG-type main sequence star that may be evolving into asubgiant as the hydrogen at its core runs out. The estimated mass of the star is 15% greater than theSun's mass,[8] and it is larger in girth than the Sun by +52%.[9] It is spinning with aprojected rotational velocity of 4 km/s.[11] The star is radiating almost three[2] times theluminosity of the Sun from itsphotosphere at aneffective temperature of 5,859 K,[4] giving it the yellow-hued glow of aG-type star.[16]

15 Leonis Minoris presents a significantly difference onproper motion measurements taken by theHipparcos andGaia spacecrafts, suggesting it may have an orbiting giant planet.[10]

References

[edit]
  1. ^Hoffleit, D. (1979), "Discordances in Star Designations",Bulletin d'Information du Centre de Données Stellaires,17: 38,Bibcode:1979BICDS..17...38H.
  2. ^abcdefgBrown, 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 atVizieR.
  3. ^abcAnderson, 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.
  4. ^abcdefGray, 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.
  5. ^Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)",SIMBAD Astronomical Database,Bibcode:1986EgUBV........0M.
  6. ^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.
  7. ^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.
  8. ^abRamírez, 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.
  9. ^abTakeda, 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.
  10. ^abcPainter, Katie E.; Bowler, Brendan P.; Franson, Kyle; Becker, Juliette C.; Burt, Jennifer A. (2025-06-26), "Astrometric Accelerations of Provisional Targets for the Habitable Worlds Observatory",The Astronomical Journal,arXiv:2506.21768.
  11. ^abMartínez-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 fromthe original(PDF) on 2017-09-22, retrieved2018-11-04.
  12. ^abBallering, 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.
  13. ^"* 15 LMi",SIMBAD,Centre de données astronomiques de Strasbourg, retrieved2016-07-19.
  14. ^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.
  15. ^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.
  16. ^"The Colour of Stars",Australia Telescope, Outreach and Education,Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived fromthe original on March 18, 2012, retrieved2016-07-25.
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