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Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Aquarius |
Right ascension | 23h 08m 19.55110s[2] |
Declination | 15° 24′ 35.7682″[2] |
Apparent magnitude (V) | 10.99±0.02[3] 10.72 - 10.94[4] |
Characteristics | |
Evolutionary stage | Main sequence |
Spectral type | M0Ve[5] |
U−B color index | +1.118[6] |
B−V color index | +1.31[3] |
Variable type | BY Dra + UV Cet[4] |
Astrometry | |
Radial velocity (Rv) | +2.7±1.6[7] km/s |
Proper motion (μ) | RA: 106.955[2] mas/yr Dec.: −18.738[2] mas/yr |
Parallax (π) | 40.1410 ± 0.0436 mas[2] |
Distance | 81.25 ± 0.09 ly (24.91 ± 0.03 pc) |
Absolute magnitude (MV) | +9.13[6] |
Details[3] | |
Mass | 0.57±0.07 M☉ |
Radius | 0.53±0.04 R☉ |
Luminosity | 0.05±0.01 L☉ |
Temperature | 3,800±76 K |
Metallicity [Fe/H] | 0.27±0.12 dex |
Rotation | 0.4307 d[8] |
Rotational velocity (v sin i) | 69.0±0.1 km/s[9] km/s |
Age | 30–40[10] Myr |
Other designations | |
Database references | |
SIMBAD | data |
HK Aquarii is a single[8] variable star in the equatorial constellation of Aquarius. It is invisible to the naked eye, having an average apparent visual magnitude that fluctuates around 10.99.[3] The star is located at a distance of 81 light years from the Sun based on parallax.[2] The radial velocity is poorly constrained but it appears to be drifting further away at a rate of ~2 km/s.[7]
This is a small red dwarf star; an M-type main-sequence star with a stellar classification of M0Ve,[5] where the 'e' indicates emission lines in the spectrum. It has 57% of the mass of the Sun and has 53% of the Sun's girth. The star is spinning with a projected rotational velocity of 69 km/s[9] and has a rotation period of just 10.34 hours.[8] Based on the abundance of iron in the atmosphere, it has a high metallicity; what astronomers term the abundances of elements with a higher atomic number than helium. The star is radiating around 5% of the luminosity of the Sun from its photosphere at an effective temperature of 3,800 K.[3]
HK Aquarii is classified as a BY Draconis variable and has been observed ranging in brightness from visual magnitude 10.72 down to 10.94.[4] This star is noteworthy for being unusually active for an isolated red dwarf; it rotates rapidly, generating a strong magnetic field that creates large starspots and powerful flares.[11] Star spots have been reported at a variety of latitudes, but not at the poles.[12] Flaring activity was reported in 1987, and a steady X-ray emission has been detected.[9] These are characteristic of very young stars; although it is not close to any youthful open cluster, it is a possible ejected member of the Pleiades.[11] (A 2016 study instead suggests it is a member of the Octans association.[10])
The signature of prominences has been detected in the star's atmosphere. These display evidence of periodic oscillations and can reach altitudes greater than two-third's of the star's radius. The prominences can obtain a higher mass and volume compared to similar features on the Sun.[13]
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