HD 36584
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Dorado |
| A | |
| Right ascension | 05h 26m 59.80322s |
| Declination | −68° 37′ 21.1327″ |
| Apparent magnitude (V) | 6.62±0.01 |
| B | |
| Right ascension | 05h 26m 59.87970s |
| Declination | −68° 37′ 22.4439″ |
| Apparent magnitude (V) | 6.91±0.01 |
| Characteristics | |
| Spectral type | F0 IV/V |
| A | |
| B−V color index | +0.37 |
| B | |
| B−V color index | +0.40 |
| Astrometry | |
| Radial velocity (Rv) | −4.60±3.4 km/s |
| Absolute magnitude (MV) | +1.57 |
| A | |
| Proper motion (μ) | RA: −10.638 mas/yr Dec.: −17.846 mas/yr |
| Parallax (π) | 12.4037±0.0261 mas |
| Distance | 263.0 ± 0.6 ly (80.6 ± 0.2 pc) |
| B | |
| Proper motion (μ) | RA: −4.710 mas/yr Dec.: −19.675 mas/yr |
| Parallax (π) | 12.4171 ± 0.0384 mas |
| Distance | 262.7 ± 0.8 ly (80.5 ± 0.2 pc) |
| Orbit | |
| Period (P) | 795 yr |
| Semi-major axis (a) | 1.704″ |
| Eccentricity (e) | 0.887 |
| Inclination (i) | 129.5° |
| Longitude of the node (Ω) | 74.8° |
| Periastron epoch (T) | 2,403,927.97472 JD |
| Argument of periastron (ω) (secondary) | 112.8° |
| Details | |
| A | |
| Mass | 1.69 M☉ |
| B | |
| Mass | 1.57 M☉ |
| Other designations | |
| 24 G. Doradus, CD−68°308, CPD−68°375, GC 6795, HD 36584, HIP 25482, HR 1859, SAO 249281, CCDM J05270-6837AB, WDS J05270-6837AB | |
| Database references | |
| SIMBAD | the system |
| A | |
| B | |
HD 36584 (HR 1859; 24 G. Doradus) is a visual binary located in the southern constellation Dorado. The primary has an apparent magnitude of 6.62 and the secondary has an apparent magnitude of 6.91, making both stars visible in a telescope but not to the naked eye. The system is located relatively close at a distance of 263 light-years based on Gaia DR3 parallax measurements and it is drifting closer with a heliocentric radial velocity of −4.6 km/s. The system has a combined absolute magnitude of 1.57.
HD 36584 was first discovered to be a double star in 1898 by astronomer R.T.A Innes. At the time of discovery, the components had a separation of only half an arcsecond and the secondary was located at a position angle of 210°. The separation between the components increased to 1.34" and the position angle of the secondary shifted to 162° in 1997. At this separation, the components can be resolved in an amateur telescope, but the individual characteristics of both stars cannot be studied. As of 2015, the secondary is located at a distance of 1.4" along a position angle of 159°. The two stars take about 795 years to circle each other in a very eccentric orbit.
The system has a combined stellar classification of F0 IV/V, indicating that it is an evolved F-type star that has the blended luminosity class of a subgiant and main sequence star. The components have masses 1.69 and 1.57 times that of the Sun respectively.