| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Andromeda |
| Right ascension | 01h 38m 31.82552s[2] |
| Declination | +45° 23′ 58.9357″[2] |
| Apparent magnitude (V) | 6.36[3] |
| Characteristics | |
| Spectral type | B9 pe[4] |
| U−Bcolor index | -0.10[3] |
| B−Vcolor index | +0.04[3] |
| Variable type | α2 CVn |
| Astrometry | |
| Radial velocity (Rv) | +3.0[5] km/s |
| Proper motion (μ) | RA: −17.292(211)[2]mas/yr Dec.: −1.386(150)[2]mas/yr |
| Parallax (π) | 7.1093±0.1589 mas[2] |
| Distance | 460 ± 10 ly (141 ± 3 pc) |
| Absolute magnitude (MV) | +0.68[6] |
| Details | |
| Mass | 2.47 ± 0.15[6] M☉ |
| Radius | 2.6 ± 0.4[6] R☉ |
| Luminosity | 52[6] L☉ |
| Surface gravity (log g) | 4.01 ± 0.14[6] cgs |
| Temperature | 10,723[7] K |
| Metallicity[Fe/H] | 0.86[7] dex |
| Rotational velocity (v sin i) | 31[8] km/s |
| Orbit[9] | |
| Companion | GY And B |
| Period (P) | 272.99 days |
| Semi-major axis (a) | > 0.25 AU |
| Eccentricity (e) | 0.47 |
| Argument of periastron (ω) (secondary) | 17.7° |
| Other designations | |
| BD +44°341,HD 9996,HIP 7651,HR 465,SAO 37393,PPM 44258[4] | |
| Database references | |
| SIMBAD | data |
GY Andromedae (GY And) is anα2 Canum Venaticorum typebinaryvariable star in the northernconstellationAndromeda. Its brightness fluctuates invisual magnitude between 6.27m and 6.41m, making it a challenge to view with the naked eye even ingood seeing conditions. Themagnetic activity on this star shows an unusually long period of variability, cycling about once every 23 years.[10] Based uponparallax measurements, this star is located at a distance of about 460light-years (140parsecs) from theEarth.[2]
This isclassified as anAp/Bp star, with apeculiar spectrum[10] showinglines ofchromium andeuropium that change in intensity over a period matching the variability cycle, although opposite inphase.[11] Its most striking characteristic is the presence of the unstable elementpromethium in itsemission spectrum. All isotopes of this element areradioactive withhalf lives of 17.7 years or less. The promethium in the outer envelope may be generated by the spontaneousfission of higher masstransuranic elements.[12]
Based onradial velocity measurements taken at theDominion Astrophysical Observatory between 1927 and 1935 Canadian astronomerWilliam Edmund Harper strongly suspected that this star was aspectroscopic binary.[13] In 1958, American astronomerHorace W. Babcock confirmed the binary nature of the star.[14] It has an orbital period of 273 days with a largeeccentricity of 0.47. The two components are separated by an estimated distance of at least3.74 × 107 km, or 0.25Astronomical Units.[9]