| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 07h01m 21.41899s[1] |
| Declination | +70° 48′ 29.8635″[1] |
| Apparent magnitude (V) | 5.69±0.01[2] |
| Characteristics | |
| Evolutionary stage | red giant branch[3] |
| Spectral type | K4 III[4] |
| U−B color index | +1.52[2] |
| B−V color index | +1.34[2] |
| Astrometry | |
| Radial velocity (Rv) | −17.8±0.2[5] km/s |
| Proper motion (μ) | RA: +13.101 mas/yr[1] Dec.: −15.749 mas/yr[1] |
| Parallax (π) | 6.3572 ± 0.0481 mas[1] |
| Distance | 513 ± 4 ly (157 ± 1 pc) |
| Absolute magnitude (MV) | −0.27[6] |
| Details | |
| Mass | 1.32±0.82[7] M☉ |
| Radius | 30.43[8] R☉ |
| Luminosity | 203±3[1] L☉ |
| Surface gravity (log g) | 1.99[9] cgs |
| Temperature | 4,396±122[10] K |
| Metallicity [Fe/H] | +0.01[9] dex |
| Age | 292[1] Myr |
| Other designations | |
AG+70°299, BD+70°430, GC 9152, HD 50885, HIP 33827, HR 2581, SAO 6041, WDS J07014+7049A[11] | |
| Database references | |
| SIMBAD | data |
HD 50885, also known as HR 2581, is a star located in the northern circumpolar constellation Camelopardalis, the giraffe. It has an apparent magnitude of 5.69,[2] making it faintly visible to the naked eye if viewed under ideal conditions. Based on parallax measurements from Gaia DR3, the object is estimated to be 513 light years distant.[1] It appears to be approaching the Solar System with a heliocentric radial velocityof−17.8 km/s.[5]
This is a solitary,[12] evolved red giant star with a stellar classification of K4 III.[4] It is currently on the red giant branch,[3] fusing a hydrogen shell around an inert helium core. It has 1.32 times the mass of the Sun[7] but has expanded to 30.4 times its girth.[8] It radiates 203 times the luminosity of the Sun[1] from its photosphere at an effective temperatureof4,396 K.[10] HD 50885 has an iron abundance only 102% that of the Sun, placing it at solar metallicity.[9]
There is an optical companion located 119″ away along a position angle of 357°.[13] This object was first noticed by Robert S. Ball in 1879[14]
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