YZ Canis Minoris

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YZ Canis Minoris
Observation data
Epoch J2000      Equinox J2000
Constellation Canis Minor
Right ascension  07h 44m 40.17262s[1]
Declination +03° 33′ 08.8778″[1]
Apparent magnitude (V) 11.15[2]
Spectral type M5 V[3]
B−V color index 1.61[2]
Radial velocity (Rv)+26.53±0.30[4] km/s
Proper motion (μ) RA: −348.103[1] mas/yr
Dec.: −445.878[1] mas/yr
Parallax (π)167.0186 ± 0.0592[1] mas
Distance19.528 ± 0.007 ly
(5.987 ± 0.002 pc)
Absolute magnitude (MV)12.32[5]
Mass0.308[6] M
Radius0.324[6] R
Surface gravity (log g)5.0[7] cgs
Temperature3,125±61[8] K
Metallicity [Fe/H]−0.26±0.08[8] dex
Rotation2.8[6] days
Other designations
YZ CMI, BD+35° 2496, GJ 285, HIP 37766, SAO 63793, G 50-4, G 112-46, LFT 547, LHS 1943, LSPM J0744+0333, LTT 12064, NLTT 18373, PLX 1827, PM 07421+0341, Ross 882, TYC 183-2190-1, GSC 00183-02190, IRAS 07420+0340, 2MASS J07444018+0333089[9]
Database references

YZ Canis Minoris is a red-hued star in the equatorial constellation of Canis Minor. With an apparent visual magnitude of 11.15,[2] it is much too faint to be viewed with the naked eye. The distance to YZ CMi can be estimated from its annual parallax shift of 167.02 mas,[1] yielding a value of 19.5 light years. Presently the star is moving further away with a heliocentric radial velocity of +26.5 km/s.[4] It made its closest approach some 162,000 years ago when it made perihelion passage at a distance of 10.2 ly.[10] YZ CMi is a potential member of the Beta Pictoris moving group.[11]

This is a red dwarf star, or M-type main-sequence star, with a stellar classification of M5 V,[3] it is a flare star, so called due to its solar flares being more powerful than those of Earth's star, and is roughly three times the size of Jupiter.[12] The radio emission from the star is in a 50 mHz bandwidth and is centered on 1464.9 mHz.[13] The X-ray surface flux is 2.73×106 erg s−1 cm−2. It has a coronal temperature of 5.79 MK.[14]


  1. ^ a b c d e f 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.
  2. ^ a b c Astudillo-Defru, N.; et al. (April 2017). "Magnetic activity in the HARPS M dwarf sample. The rotation-activity relationship for very low-mass stars through R'(HK)". Astronomy & Astrophysics. 600: 15. Bibcode:2017A&A...600A..13A. doi:10.1051/0004-6361/201527078. A13.
  3. ^ a b 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. arXiv:1509.01590. Bibcode:2015ApJ...812....3W. doi:10.1088/0004-637X/812/1/3. 3.
  4. ^ a b 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.
  5. ^ 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.
  6. ^ a b c Newton, Elisabeth R.; et al. (January 2017). "The Hα Emission of Nearby M Dwarfs and its Relation to Stellar Rotation". The Astrophysical Journal. 834 (1): 13. Bibcode:2017ApJ...834...85N. doi:10.3847/1538-4357/834/1/85. 85.
  7. ^ Lépine, Sébastien; et al. (2013). "A Spectroscopic Catalog of the Brightest (J < 9) M Dwarfs in the Northern Sky". The Astronomical Journal. 145 (4): 102. arXiv:1206.5991. Bibcode:2013AJ....145..102L. doi:10.1088/0004-6256/145/4/102.
  8. ^ a b Gaidos, Eric; Mann, Andrew W. (August 2014). "M dwarf metallicities and giant planet occurrence: ironing out uncertainties and systematics". The Astrophysical Journal. 791 (1): 9. arXiv:1406.4071. Bibcode:2014ApJ...791...54G. doi:10.1088/0004-637X/791/1/54. 54.
  9. ^ "YZ CMi". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 26 August 2018.
  10. ^ Bailer-Jones, C. A. L. (March 2015). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: 13. arXiv:1412.3648. Bibcode:2015A&A...575A..35B. doi:10.1051/0004-6361/201425221. A35.
  11. ^ Nakajima, Tadashi; Morino, Jun-Ichi (January 2012). "Potential Members of Stellar Kinematic Groups within 30 pc of the Sun". The Astronomical Journal. 143 (1): 2. Bibcode:2012AJ....143....2N. doi:10.1088/0004-6256/143/1/2.
  12. ^ "First flares on a distant star". New Scientist: 305. February 4, 1982.
  13. ^ Lang, K. R. (October 23–27, 1989). "Flare stars at radio wavelengths". In Mirzoyan, L.V. (ed.). Flare Stars in Star Clusters, Associations, and the Solar Vicinity: Proceedings of the 137th Symposium of the International Astronomical Union. Byurakan (Armenia), U.S.S.R.: Springer (published 1990). pp. 127–130. ISBN 978-0-7923-0771-6.CS1 maint: Date format (link)
  14. ^ Johnstone, C. P.; Güdel, M. (June 2015), "The coronal temperatures of low-mass main-sequence stars", Astronomy & Astrophysics, 578: 4, arXiv:1505.00643, Bibcode:2015A&A...578A.129J, doi:10.1051/0004-6361/201425283, A129