15 Leonis Minoris

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15 Leonis Minoris
Ursa Major constellation map.svg
Red circle.svg
Location of 15 Leo Minoris (circled)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Ursa Major [1]
Right ascension 09h 48m 35.37130s [2]
Declination +46° 01′ 15.6338″ [2]
Apparent magnitude  (V)5.08 [3]
Characteristics
Spectral type G0 IV-V [4]
U−B color index +0.175 [5]
B−V color index 0.619±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]
Distance 61.7 ± 0.1  ly
(18.90 ± 0.05  pc)
Absolute magnitude  (MV)3.75 [7]
Details
Mass 1.15 [8]   M☉
Radius 1.52 [9]   R☉
Luminosity 2.912±0.010 [2]   L☉
Surface gravity (log g)4.04 [4]   cgs
Temperature 5,859 [4]   K
Metallicity [Fe/H]0.01 [4]   dex
Rotational velocity (v sin i)3.97 [10]  km/s
Age 9.3 [11]   Gyr
Other designations
15 LMi, BD+46°1551, FK5 1255, GJ 368, HD 84737, HIP 48113, HR 3881, SAO 43046 [12]
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

  1. ↑ Hoffleit, D. (1979), "Discordances in Star Designations", Bulletin d'Information du Centre de Données Stellaires, 17: 38, Bibcode:1979BICDS..17...38H.
  2. 1 2 3 4 5 6 7 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.
  3. 1 2 3 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.
  4. 1 2 3 4 5 6 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.
  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. 1 2 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.
  9. 1 2 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.
  10. 1 2 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.
  11. 1 2 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.
  12. ↑ "* 15 LMi", SIMBAD , Centre de données astronomiques de Strasbourg , retrieved 2016-07-19.
  13. ↑ 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.
  14. ↑ 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.
  15. ↑ "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.
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