Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Lepus |
Right ascension | 05h 44m 26.537s [2] |
Declination | −22° 25′ 18.61″ [2] |
Apparent magnitude (V) | 6.141 [3] |
Characteristics | |
Spectral type | K2V [4] |
U−B color index | +0.74 [5] |
B−V color index | +0.96 [5] |
Variable type | BY Draconis [4] |
Astrometry | |
Radial velocity (Rv) | −9.80±0.12 [2] km/s |
Proper motion (μ) | RA: −304.905 [2] mas/yr Dec.: −352.606 [2] mas/yr |
Parallax (π) | 112.4661±0.0151 mas [2] |
Distance | 29.000 ± 0.004 ly (8.892 ± 0.001 pc) |
Absolute magnitude (MV) | 6.31 [3] |
Details | |
Mass | 0.800+0.040 −0.048 [2] M☉ |
Radius | 0.793±0.017 [2] R☉ |
Luminosity | 0.300±0.005 [2] L☉ |
Surface gravity (log g) | 4.66±0.01 [6] cgs |
Temperature | 4,869±61 [6] K |
Metallicity [Fe/H] | 0.01±0.06 [6] dex |
Rotational velocity (v sin i) | 2.8±1.8 [7] km/s |
Age | 0.9 [8] Gyr |
Other designations | |
γ Lep B, AK Lep, BD−22 1210, GJ 216 B, HD 38392, HR 1982, SAO 170757, LTT 2363 [9] | |
Database references | |
SIMBAD | data |
AK Leporis, also known as Gamma Leporis B, is a variable star in the southern constellation of Lepus the hare. It has an apparent visual magnitude of 6.141, [3] so, according to the Bortle scale, it is faintly visible from rural skies at night. This star forms a wide binary star system with Gamma Leporis—the two have an angular separation of 97″, making them difficult to separate with the naked eye even under the best conditions. [10] [11] Both Gamma Leporis and AK Leporis are members of the Ursa Major Moving Group of stars that share a common motion through space. [7]
This is a BY Draconis variable star that undergoes slight brightness variations due to stellar activity. Differential rotation causes changes to the periodicity of the variation depending on the latitude of the activity. [4] X-ray emission has been detected from AK Leporis, and it is located at or near a radio source. [12]
Infrared observation of this star shows a large excess at a wavelength of 24 μm. This may be explained by the proximity of Gamma Leporis to the line of sight, or there may be a red dwarf companion or a dust disc. There is no excess observed at 70 μm. [8]