| Observation data EpochJ2000.0 EquinoxJ2000.0 | |
|---|---|
| Constellation | Ursa Major[1] |
| Right ascension | 12h 48m 39.44700s[2] |
| Declination | 60° 19′ 11.0379″[2] |
| Apparent magnitude (V) | 5.85[3] |
| Characteristics | |
| Evolutionary stage | main sequence[4] |
| Spectral type | F7 V[5] |
| U−Bcolor index | −0.04[3] |
| B−Vcolor index | +0.46[3] |
| Astrometry | |
| Radial velocity (Rv) | −18.0±0.9[6] km/s |
| Proper motion (μ) | RA: +120.949[2]mas/yr Dec.: +35.712[2]mas/yr |
| Parallax (π) | 38.1905±0.2904 mas[2] |
| Distance | 85.4 ± 0.6 ly (26.2 ± 0.2 pc) |
| Absolute magnitude (MV) | +4.2±0.2[4] |
| Details | |
| Mass | 1.4[7] M☉ |
| Radius | 1.22[4] R☉ |
| Luminosity | 6.45[1] L☉ |
| Surface gravity (log g) | 4.5[4] cgs |
| Temperature | 6,400[4] K |
| Metallicity [Fe/H] | −0.19[8] dex |
| Rotation | 14.7[9] days |
| Rotational velocity (v sin i) | 41.5±1.1[4] km/s |
| Age | 300−400[4] Myr |
| Other designations | |
| BD+61°1320,GJ 9417,HD 111456,HIP 62512,HR 4867,SAO 236405,WDS J12487+6019AB[10] | |
| Database references | |
| SIMBAD | data |
HD 111456 is a yellow-white huedstar in the northerncircumpolar constellation ofUrsa Major. It is dimly visible to the naked eye, having anapparent visual magnitude of 5.85.[3] Based upon an annualparallax shift of38.2 mas as seen from Earth, it is located about85 light years from theSun. The star is moving closer to the Sun with aradial velocity of−18 km/s.[6] HD 111456 is a nucleus cluster member of theUrsa Major Moving Group, a set of stars that are moving through space with a similar heading and velocity. Six other stars in the nucleus of the group are prominent members of theBig Dipperasterism.[5]
Thestellar classification for this star is F7 V,[5] indicating that it is an ordinaryF-type main-sequence star. It is young, around 300−400 million years of age, and is spinning with a relatively highprojected rotational velocity of 41.5 km/s.[4] This is one of the mostactive F-type stars known, and it is a strong emitter ofX-rays[4] and an extremeUV source. It is anastrometric binary with a period of four years and a mass ratio of 0.5. Hence, the companion may be a youngwhite dwarf star.[11]
