  | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Camelopardalis [1] |
| Right ascension | 04h 21m 47.64917s [2] |
| Declination | +60° 44′ 08.2461″ [2] |
| Apparent magnitude (V) | 5.40±0.01 [3] |
| Characteristics | |
| Spectral type | M0 III [4] |
| B−V color index | +1.50 [5] |
| Variable type | suspected [6] |
| Astrometry | |
| Radial velocity (Rv) | +25.2±0.3 [7] km/s |
| Proper motion (μ) | RA: +55.890 mas/yr [2] Dec.: −114.046 mas/yr [2] |
| Parallax (π) | 5.3716±0.0848 mas [2] |
| Distance | 607 ± 10 ly (186 ± 3 pc) |
| Absolute magnitude (MV) | −0.27 [1] |
| Details | |
| Mass | 1.18 [8] M☉ |
| Radius | 52.8±2.7 [9] R☉ |
| Luminosity | 570±16 [10] L☉ |
| Surface gravity (log g) | 1.29 [11] cgs |
| Temperature | 4,033±122 [12] K |
| Metallicity [Fe/H] | +0.11 [8] dex |
| Other designations | |
| 25 H. Camelopardalis, [13] NSV 1558, AG+60°426, BD+60°800, FK5 2317, GC 5244, HD 27245, HIP 20376, HR 1335, SAO 13113 [14] | |
| Database references | |
| SIMBAD | data |
HD 27245, also known as HR 1335 or rarely 25 H. Camelopardalis is a solitary red-hued star [15] located in the northern circumpolar constellation Camelopardalis. It has an apparent magnitude of 5.4, [3] making it faintly visible to the naked eye. Gaia DR3 Parallax measurements place it approximately 607 light years [2] away from it the Solar System and is drifting further away with a heliocentric radial velocity of 25.2 km/s . [7] At its current distance, HD 27245's brightness is diminished by 0.36 magnitudes due to extinction from interstellar dust. [16] It has an absolute magnitude of −0.27. [1]
HD 27245 is an aging red giant with a stellar classification of M0 III. [4] It has 118% the mass of the Sun [8] but has expanded to a radius of 52.8 R☉. [11] It radiates 570 times the luminosity of the Sun [10] from its enlarged photosphere at an effective temperature of 4,033 K . [12] HD 27245's iron abundance is 129% that of the Sun's, [8] making it metal enriched.
HD 27245 is a suspected variable star with an amplitude of 0.05 magnitudes. [6] Its variability was first observed in 1930 by Joel Stebbins. [17] However, Eggen (1967) instead lists it as an ordinary M-type giant and used the object for comparison. [18] In 1978–9, HD 28245 was again listed as a variable star but did not provide further insight. [19] As of 2017, the star has not been confirmed to be variable. [6]
