Eta Andromedae
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 00h 57m 12.400s |
| Declination | +23° 25′ 03.54″ |
| Apparent magnitude (V) | 4.403 |
| Characteristics | |
| Spectral type | G8III-IV + G8III-IV |
| U−B color index | +0.69 |
| B−V color index | +0.94 |
| R−I color index | +0.48 |
| Astrometry | |
| η And A | |
| Radial velocity (Rv) | −10.30±0.29 km/s |
| Proper motion (μ) | RA: −43.008 mas/yr Dec.: −45.254 mas/yr |
| Parallax (π) | 12.5624±0.2525 mas |
| Distance | 260 ± 5 ly (80 ± 2 pc) |
| Absolute magnitude (MV) | 0.52±0.06 |
| η And B | |
| Absolute magnitude (MV) | 1.07±0.07 |
| Orbit | |
| Period (P) | 115.72±0.01 d |
| Semi-major axis (a) | 10.37±0.03 mas |
| Eccentricity (e) | 0.006±0.002 |
| Inclination (i) | 30.5±0.4° |
| Longitude of the node (Ω) | 69.4±0.5° |
| Periastron epoch (T) | 48013±1 MJD |
| Argument of periastron (ω) (secondary) | 215±4° |
| Details | |
| η And A | |
| Mass | 2.6±0.35 M☉ |
| Radius | 10.7 R☉ |
| Luminosity (bolometric) | 65±3 L☉ |
| Surface gravity (log g) | 2.8 cgs |
| Temperature | 4,900 K |
| Age | 800 Myr |
| η And B | |
| Mass | 2.3±0.31 M☉ |
| Radius | 8.6 R☉ |
| Luminosity (bolometric) | 39±3 L☉ |
| Surface gravity (log g) | 3.0 cgs |
| Temperature | 4,900 K |
| Other designations | |
| Kui, η Andromedae, η And, Eta And, 38 Andromedae, 38 And, BD+22°153, FK5 2060, GC 1136, HD 5516, HIP 4463, HR 271, SAO 74388, PPM 90327, CCDM J00572+2325A, WDS 00572+2325A/Aa | |
| Database references | |
| SIMBAD | data |
Eta Andromedae, also named Kui, is a spectroscopic binary star system in the northern constellation of Andromeda. It consists of two G-type evolved stars orbiting each other with a period of 115.7 days and has an overall apparent visual magnitude of approximately 4.403. Based on parallax measurements, this system is located at a distance of approximately 260 light years from the Sun. But it is drawing closer with a heliocentric radial velocity of −10.30 km/s.
This star was discovered to be a double-lined spectroscopic binary in a series of spectra taken in 1899 and 1900. Its orbit was computed in 1946 from spectroscopic observations. Because spectroscopy only reveals the radial velocity of a star towards or away from the viewer, such a computation does not determine all orbital elements. In observations made from 1990 to 1992, Eta Andromedae was resolved interferometrically by the Mark III Stellar Interferometer at Mount Wilson Observatory, California, United States. This allowed a more complete orbit to be computed and, in 1993, published.
The primary component has 2.6 times the mass of the Sun and 10.7 times the Sun's radius. It is radiating 65 times the Sun's luminosity from its enlarged photosphere at an effective temperature of 4,900 K. The fainter secondary member has 2.3 times the mass and 8.6 times the radius of the Sun. It radiates 39 times the luminosity of the Sun at a temperature of 4,900 K.
Eta Andromedae has a visual companion star of apparent visual magnitude 11.5, BD+22°153B, visible 129.2 arcseconds away.