Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
---|---|
Constellation | Corona Australis |
Right ascension | 18h 56m 16.95125s[1] |
Declination | −42° 42′ 38.4231″[1] |
Apparent magnitude (V) | 5.35±0.01[2] |
Characteristics | |
Spectral type | K0 III[3] or G6 III-IV[4] |
B−V color index | +1.00[5] |
Astrometry | |
Radial velocity (Rv) | −21.1±0.8[6] km/s |
Proper motion (μ) | RA: −27.046 mas/yr Dec.: −29.284 mas/yr |
Parallax (π) | 10.3847 ± 0.109 mas[1] |
Distance | 314 ± 3 ly (96 ± 1 pc) |
Absolute magnitude (MV) | +0.57[7] |
Details | |
Mass | 1.93±0.21[8] M☉ |
Radius | 12.3±0.2[8] R☉ |
Luminosity | 76.3±2.0[8] L☉ |
Surface gravity (log g) | 2.55±0.07[8] cgs |
Temperature | 4,877±26[8] K |
Metallicity [Fe/H] | −0.28±0.02[8] dex |
Rotational velocity (v sin i) | <1[9] km/s |
Age | 346[1] Myr |
Other designations | |
Database references | |
SIMBAD | data |
HD 175219, also known as HR 7122, is a solitary,[12] orange hued star located in the southern constellation Corona Australis. It has an apparent magnitude of 5.35,[2] allowing it to be faintly visible to the naked eye. The object is located relatively close at a distance of 314 light years based on Gaia DR3 parallax measurements[1] but is drifting closer with a heliocentric radial velocity of −21.1 km/s.[6] At its current distance, HD 175219's brightness is diminished by 0.26 magnitudes due to interstellar dust.[13] It has an absolute magnitude of +0.57.[7]
This is a red giant with a stellar classification of K0 III.[3] An earlier source gives it a class of G6 III-IV,[4] indicating that it is an evolved G-type star with a luminosity class intermediate between a giant star and a subgiant. At present it has nearly twice the mass of the Sun but it has expanded to 12.3 times the Sun's radius.[8] HD 175219 radiates 76.3 times the luminosity of the Sun from its enlarged photosphere at an effective temperature of 4,877 K.[8] The star is metal deficient, having less than half the abundance of heavy elements compared to the Sun.[8] Common for giant stars, it spins slowly, having a projected rotational velocity too low to be measured accurately.[9]