ADS 48
Triple star system in the constellation of Andromeda
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ADS 48 is a binary system in the constellation of Andromeda.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Andromeda[1] |
| ADS 48 A | |
| Right ascension | 00h 05m 41.0219s[2] |
| Declination | +45° 48′ 43.545″[2] |
| Apparent magnitude (V) | 8.826[3] |
| ADS 48 B | |
| Right ascension | 00h 05m 41.0028s[4] |
| Declination | +45° 48′ 37.354″[4] |
| Apparent magnitude (V) | 8.995[3] |
| Characteristics | |
| ADS 48 A | |
| Spectral type | K6V[5] |
| B−V color index | +1.344[3] |
| ADS 48 B | |
| Spectral type | M0.5V[5] |
| B−V color index | +1.345[3] |
| Astrometry | |
| Radial velocity (Rv) | 1.49±0.1[6] km/s |
| Proper motion (μ) | RA: 887.48±1.02[7] mas/yr Dec.: −152.02±1.04[7] mas/yr |
| Parallax (π) | 88.44±1.56 mas[7] |
| Distance | 36.9 ± 0.7 ly (11.3 ± 0.2 pc) |
| Absolute magnitude (MV) | +7.93[1] |
| Orbit[8] | |
| Period (P) | 557±120 yr |
| Semi-major axis (a) | 74±10 AU |
| Eccentricity (e) | 0.19±0.08 |
| Inclination (i) | 54.3±2.3° |
| Longitude of the node (Ω) | 12.5±2.8° |
| Periastron epoch (T) | 2110±30 |
| Argument of periastron (ω) (secondary) | 256±31° |
| Details | |
| ADS 48 A | |
| Mass | 0.50[9] M☉ |
| ADS 48 B | |
| Mass | 0.53[9] M☉ |
| Other designations | |
| HD 38, HIP 473, GJ 4, CCDM J00057+4548AB, WDS J00057+4549AB | |
| ADS 48 A: HD 38A, SAO 36046, GC 71, GJ 4 A, CCDM J00057+4548A, WDS J00057+4549A | |
| ADS 48 B: HD 38B, SAO 36048, GC 72, GJ 4 B, CCDM J00057+4548B, WDS J00057+4549B | |
| Database references | |
| SIMBAD | AB |
| A | |
| B | |
The components have apparent visual magnitudes of 8.826 and 8.995.[3] Component A is a K-type main-sequence star, while component B is an M-type main-sequence star (red dwarf).[5] The stars are orbiting with a period of 550 years and a separation of 74 AU.[8]
Multiple stars lie close to ADS 48 in the line of sight, and have been considered components C, D and E of the system, but are background objects. ADS 48 F (Gliese 2) is at a similar distance from the pair and share similar proper motions, but is moving faster than the escape velocity of the pair and thus is not gravitationally bound.[10] The existence of an unseen companion of 0.05 M☉ has also been proposed,[9] but this was refuted.[8]