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]
Maehara
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