YZ Canis Minoris

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YZ Canis Minoris
YZCMiLightCurve.png
A light curve for YZ Canis Minoris from TESS data, adapted from Maehara et al.(2021).[1] The main plot shows both the periodic brightness variation and several flares. The inset plot shows the strongest flare with an expanded time scale.
Observation data
Epoch J2000      Equinox J2000
Constellation Canis Minor
Right ascension 07h 44m 40.17262s[2]
Declination +03° 33′ 08.8778″[2]
Apparent magnitude (V) 11.15[3]
Characteristics
Spectral type M5 V[4]
B−V color index 1.61[3]
Astrometry
Radial velocity (Rv)+26.53±0.30[5] km/s
Proper motion (μ) RA: −348.103[2] mas/yr
Dec.: −445.878[2] mas/yr
Parallax (π)166.9769 ± 0.0343[6] mas
Distance19.533 ± 0.004 ly
(5.989 ± 0.001 pc)
Absolute magnitude (MV)12.32[7]
Details
Mass0.308[8] M☉
Radius0.324[8] R☉
Surface gravity (log g)5.0[9] cgs
Temperature3,125±61[10] K
Metallicity [Fe/H]−0.26±0.08[10] dex
Rotation2.8[8] days
Other designations
YZ CMI, BD+35° 2496, GJ 285, HIP 37766, SAO 63793, G 50-4, G 112-46, LFT 547, LHS 1943, 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[11]
Database references
SIMBADdata

YZ Canis Minoris is a red-hued star in the equatorial constellation of Canis Minor. With an apparent visual magnitude of 11.15,[3] 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,[2] 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.[5] It made its closest approach some 162,000 years ago when it made perihelion passage at a distance of 10.2 ly.[12] YZ CMi is a potential member of the Beta Pictoris moving group.[13]

This is a red dwarf star, or M-type main-sequence star, with a stellar classification of M5 V.[4] 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.[14] The radio emission from the star is in a 50 mHz bandwidth and is centered on 1464.9 mHz.[15] The X-ray surface flux is 2.73×106 erg s−1 cm−2. It has a coronal temperature of 5.79 MK.[16]

References[]

  1. ^ Maehara, Hiroyuki; Notsu, Yuta; Namekata, Kousuke; Honda, Satoshi; Kowalski, Adam F.; Katoh, Noriyuki; Ohshima, Tomohito; Iida, Kota; Oeda, Motoki; Murata, Katsuhiro L.; Yamanaka, Masayuki; Takagi, Kengo; Sasada, Mahito; Akitaya, Hiroshi; Ikuta, Kai; Okamoto, Soshi; Nogami, Daisaku; Shibata, Kazunari (February 2021). "Time-resolved spectroscopy and photometry of M dwarf flare star YZ Canis Minoris with OISTER and TESS: Blue asymmetry in the Hα line during the non-white light flare". Publications of the Astronomical Society of Japan. 73 (1): 44–65. doi:10.1093/pasj/psaa098. Retrieved 17 November 2021.
  2. ^ a b c d e 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.
  3. ^ 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. arXiv:1610.09007. Bibcode:2017A&A...600A..13A. doi:10.1051/0004-6361/201527078. S2CID 119237202. A13.
  4. ^ 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. S2CID 17434970. 3.
  5. ^ 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. S2CID 51814894.
  6. ^ Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. Gaia EDR3 record for this source at VizieR.
  7. ^ 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.
  8. ^ 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. arXiv:1611.03509. Bibcode:2017ApJ...834...85N. doi:10.3847/1538-4357/834/1/85. S2CID 55000202. 85.
  9. ^ 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. S2CID 117144290.
  10. ^ 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. S2CID 118744016. 54.
  11. ^ "YZ CMi". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 26 August 2018.
  12. ^ 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. S2CID 59039482. A35.
  13. ^ 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.
  14. ^ "First flares on a distant star". New Scientist: 305. February 4, 1982.
  15. ^ 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.
  16. ^ 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, S2CID 117151984, A129
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