HD 36848
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Columba |
| Right ascension | 05h 32m 51.4130s |
| Declination | −38° 30′ 48.1306″ |
| Apparent magnitude (V) | 5.46±0.01 |
| Characteristics | |
| Evolutionary stage | red giant branch |
| Spectral type | K2/3 III |
| B−V color index | +1.22 |
| Astrometry | |
| Radial velocity (Rv) | −0.6±0.1 km/s |
| Proper motion (μ) | RA: +48.475 mas/yr Dec.: −10.959 mas/yr |
| Parallax (π) | 18.7844±0.0462 mas |
| Distance | 173.6 ± 0.4 ly (53.2 ± 0.1 pc) |
| Absolute magnitude (MV) | +1.84 |
| Details | |
| Mass | 1.18 M☉ |
| Radius | 8.71+0.62 −0.58 R☉ |
| Luminosity | 24.54 L☉ |
| Surface gravity (log g) | 2.7±0.2 cgs |
| Temperature | 4,460±70 K |
| Metallicity [Fe/H] | +0.28±0.05 dex |
| Rotational velocity (v sin i) | <2.7 km/s |
| Age | 7.33 Gyr |
| Other designations | |
| 24 G. Columbae, CD−38°2085, CPD−38°653, GC 6889, HD 36848, HIP 25993, HR 1877, SAO 195948 | |
| Database references | |
| SIMBAD | data |
HD 36848 (HR 1877) is a star in the southern constellation Columba. It has an apparent magnitude of 5.46, allowing it to be faintly seen with a naked eye. The star is relatively close at a distance of 174 light years and is moving closer with a heliocentric radial velocity of only −0.6 km/s.
HD 36848 has a stellar classification of K2/3 III — intermediate between a K2 and 3 giant star. It is on the red giant branch, meaning it has exhausted its core hydrogen and is now fusing hydrogen in a shell outside the core. It has a comparable mass to the Sun but has expanded to 8.71 times the radius of the Sun after 7.33 billion years. It shines with a luminosity of 24.5 L☉ from its enlarged photosphere at an effective temperature of 4,460 K, giving t an orange hue. The star is metal enriched with an iron abundance 90% greater than that of the Sun and spins with a projected rotational velocity lower than 2.7 km/s.
The star's multiplicity status isn't generally agreed on. Eggleton et al. classifies it as a solitary star while De Mederios et al. finds it to be a probable spectroscopic binary.