YZ Canis Minoris
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 40.17230s[2] |
Declination | +03° 33′ 08.8752″[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: −347.782[2] mas/yr Dec.: −445.702[2] mas/yr |
Parallax (π) | 166.9769 ± 0.0343 mas[2] |
Distance | 19.533 ± 0.004 ly (5.989 ± 0.001 pc) |
Absolute magnitude (MV) | 12.32[6] |
Details | |
Mass | 0.36±0.02[7] M☉ |
Radius | 0.37±0.01[7] R☉ |
Luminosity | 1.116×10−2[7] L☉ |
Surface gravity (log g) | 5.0[8] cgs |
Temperature | 3,125±61[9] K |
Metallicity [Fe/H] | −0.26±0.08[9] dex |
Rotation | 2.8[10] days |
Rotational velocity (v sin i) | 4.0[11] km/s |
Age | 49[12] Myr |
Other designations | |
Database references | |
SIMBAD | data |
Location of YZ Canis Minoris in the constellation Canis Minor |
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 mas, 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.[14] YZ CMi is a potential member of the Beta Pictoris moving group.[15]
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 stellar flares being more powerful than those of Earth's star, and is roughly three times the size of Jupiter.[16] The radio emission from the star is in a 50 mHz bandwidth and is centered on 1464.9 mHz.[17] The X-ray surface flux is 2.73×106 erg s−1 cm−2. It has a coronal temperature of 5.79 MK.[18]
References
[edit]- ^ 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. arXiv:2009.14412. Bibcode:2021PASJ...73...44M. doi:10.1093/pasj/psaa098.
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ 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.
- ^ 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.
- ^ 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.
- ^ 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 Cifuentes, C.; Caballero, J. A.; Cortés-Contreras, M.; Montes, D.; Abellán, F. J.; Dorda, R.; Holgado, G.; Zapatero Osorio, M. R.; Morales, J. C.; Amado, P. J.; Passegger, V. M.; Quirrenbach, A.; Reiners, A.; Ribas, I.; Sanz-Forcada, J. (2020-10-01), "CARMENES input catalogue of M dwarfs. V. Luminosities, colours, and spectral energy distributions", Astronomy and Astrophysics, 642: A115, arXiv:2007.15077, Bibcode:2020A&A...642A.115C, doi:10.1051/0004-6361/202038295, ISSN 0004-6361
- ^ 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.
- ^ 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.
- ^ 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.
- ^ Reiners, Ansgar; et al. (2018). "The CARMENES search for exoplanets around M dwarfs. High-resolution optical and near-infrared spectroscopy of 324 survey stars". Astronomy and Astrophysics. 612: A49. arXiv:1711.06576. Bibcode:2018A&A...612A..49R. doi:10.1051/0004-6361/201732054. S2CID 62818673.
- ^ Meshkat, Tiffany; et al. (December 2017). "A Direct Imaging Survey of Spitzer-detected Debris Disks: Occurrence of Giant Planets in Dusty Systems". The Astronomical Journal. 154 (6): 21. arXiv:1710.04185. Bibcode:2017AJ....154..245M. doi:10.3847/1538-3881/aa8e9a. S2CID 42042014. 245.
- ^ "YZ CMi". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 26 August 2018.
- ^ 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.
- ^ 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.
- ^ "First flares on a distant star". New Scientist: 305. February 4, 1982.
- ^ 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.
- ^ 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