| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Volans |
| Right ascension | 08h44m 29.9582s[1] |
| Declination | −65° 49′ 31.550″[1] |
| Apparent magnitude (V) | 6.02±0.01[2] |
| Characteristics | |
| Evolutionary stage | main sequence[3] |
| Spectral type | A4 V[4] |
| U−B color index | +0.08[5] |
| B−V color index | +0.20[5] |
| Astrometry | |
| Radial velocity (Rv) | 10.7±0.5[6] km/s |
| Proper motion (μ) | RA: −63.156 mas/yr[1] Dec.: +103.462 mas/yr[1] |
| Parallax (π) | 17.0428 ± 0.0235 mas[1] |
| Distance | 191.4 ± 0.3 ly (58.68 ± 0.08 pc) |
| Absolute magnitude (MV) | +2.19[7] |
| Details | |
| Mass | 1.81[8] M☉ |
| Radius | 1.84±0.05[9] R☉ |
| Luminosity | 11.7±0.4[3] L☉ |
| Surface gravity (log g) | 4.33[10] cgs |
| Temperature | 7,998±272[10] K |
| Metallicity [Fe/H] | −0.06[11] dex |
| Rotational velocity (v sin i) | 96±1[12] km/s |
| Age | 630[8] Myr |
| Other designations | |
41 G. Volantis, CPD−65°1013, FK5 2691, GC 12090, HD 75171, HIP 42895, HR 3495, SAO 250317 | |
| Database references | |
| SIMBAD | data |
HD 75171, also known as HR 3495, is a solitary,[8] white hued star located in the southern constellationofVolans. It has an apparent magnitude of 6.02,[2] making it faintly visible to the naked eye under ideal conditions. The object is relatively close at a distance of 191 light years but is receding with a heliocentric radial velocityof10.7 km/s. Eggen (1995) lists it as a probable member of the Hyades Supercluster.
HD 75171 has a stellar classification of A4 V,[4] indicating that it is an ordinary A-type main-sequence star. It has also been given a cooler class of A9 V.[13] It has 1.81 times the mass of the Sun[8] and a diameter of 1.84 R☉.[9] It radiates at 12 times the luminosity of the Sun[3] from its photosphere at an effective temperatureof7,998 K.[10] Like most hot stars, it spins quickly with a projected rotational velocityof96 km/s.[12] HD 75171 is estimated to be 630 million years old,[8] well around the age of the actual Hyades cluster. Zorec and Royer (2012) model it to be a dwarf star 50.4% through its main sequence lifetime,[3] and Gaia Data Release 3 models also show a star roughly halfway through its main sequence life.[1] The star has a near solar metallicity, with the iron abundance being 87% that of the Sun.[11]
