15 Leonis Minoris
(Redirected from 15 LMi)
  | |
| 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 | |
| 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
[edit]- ^ 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.
