HD 145250
Star in the constellation Scorpius
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HD 145250 is a star in the constellation of Scorpius. At an apparent magnitude of +5.13, it is faintly visible to the naked eye in locations far from light pollution. Parallax measurements give a distance of 283 light-years. The star is inside the Upper Scorpius subgroup of the Scorpius–Centaurus association,[1] but is not a member.[8]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Scorpius[1] |
| Right ascension | 16h 11m 02.06830s[2] |
| Declination | −29° 24′ 58.3873″[2] |
| Apparent magnitude (V) | 5.13[3] |
| Characteristics | |
| Evolutionary stage | Red-giant branch[1] |
| Spectral type | K0 III[4] |
| U−B color index | 1.02[3] |
| B−V color index | 1.12[3] |
| Astrometry | |
| Radial velocity (Rv) | −26.46±0.12[2] km/s |
| Proper motion (μ) | RA: −88.148 mas/yr[2] Dec.: −87.568 mas/yr[2] |
| Parallax (π) | 11.5124±0.0934 mas[2] |
| Distance | 283 ± 2 ly (86.9 ± 0.7 pc) |
| Absolute magnitude (MV) | +0.15[5] |
| Details | |
| Mass | 1.38±0.09[1] M☉ |
| Radius | 16.5±2.7[1] R☉ |
| Luminosity | 86.2±2.1[1] L☉ |
| Surface gravity (log g) | 2.74±0.10[6] cgs |
| Temperature | 4,540±50[6] K |
| Metallicity [Fe/H] | −0.36±0.05[6] dex |
| Other designations | |
| CD−29°12343, HD 145250, HIP 79302, HR 6017, TYC 6792-2274-1[7] | |
| Database references | |
| SIMBAD | data |
The spectrum of this star matches a spectral class of K0 III,[4] with the luminosity class III indicating it is a giant star that has exhausted the hydrogen at its core. It is currently fusing hydrogen in a shell around the core, being in the evolutionary stage known as the red-giant branch. HD 145250 displays photometric variability caused by seismic oscillations, and has been studied using asteroseismology to determine its physical properties. The star has a mass 1.38 times the mass of the Sun and has expanded to 16 times the Sun's radius. It now radiates 86 times the Sun's luminosity from its photosphere[1] at an effective temperature of 4,540 K.[6] This temperature give it the orangish hue typical of a K-type star.[9]
While no companion star has been detected,[10] its proper motions derived by the Hipparcos and Gaia satellites are slightly different, suggesting it may be an astrometric binary with a low-mass companion.[11][1]