YZ Canis Minoris
Star in the constellation Canis Minor
From Wikipedia, the free encyclopedia
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 mas, yielding a value of 19.5 light-years (5.97 parsecs). Presently the star is moving further away with a heliocentric radial velocity of +25.7 km/s.[1] 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]
  YZ Location of YZ Canis Minoris in the constellation Canis Minor | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Canis Minor |
| Right ascension | 07h 44m 40.17230s[1] |
| Declination | +03° 33′ 08.8752″[1] |
| Apparent magnitude (V) | 11.15[2] |
| Characteristics | |
| Spectral type | M5 V[3] |
| B−V color index | 1.61[2] |
| Astrometry | |
| Radial velocity (Rv) | +25.72±0.20[1] km/s |
| Proper motion (μ) | RA: −347.782 mas/yr[1] Dec.: −445.702 mas/yr[1] |
| Parallax (π) | 166.9769±0.0343 mas[1] |
| Distance | 19.533 ± 0.004 ly (5.989 ± 0.001 pc) |
| Absolute magnitude (MV) | 12.32[4] |
| Details | |
| Mass | 0.36±0.02[5] M☉ |
| Radius | 0.37±0.01[5] R☉ |
| Luminosity | 1.116×10−2[5] L☉ |
| Surface gravity (log g) | 5.0[6] cgs |
| Temperature | 3,125±61[7] K |
| Metallicity [Fe/H] | −0.26±0.08[7] dex |
| Rotation | 2.8[8] days |
| Rotational velocity (v sin i) | 4.0[9] km/s |
| Age | 49[10] Myr |
| Other designations | |
| YZ CMi, GJ 285, HIP 37766, 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[11] | |
| Database references | |
| SIMBAD | data |
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 stellar flares being more powerful than those of Earth's star, and is roughly three times the size of jupiter.[15] A "megaflare" was observed on 16 January 2009, lasting for more than 7 hours. This was one of the most energetic flares observed on an isolated low-mass star.[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]