GY Andromedae

From Wikipedia, the free encyclopedia
  (Redirected from HR 465)
Jump to: navigation, search
GY Andromedae
Observation data
Epoch J2000      Equinox J2000
Constellation Andromeda
Right ascension 01h 38m 31.82463s[1]
Declination +45° 23′ 58.9324″[1]
Apparent magnitude (V) 6.36[2]
Spectral type B9 pe[3]
U−B color index -0.10[2]
B−V color index +0.04[2]
Variable type α2 CVn
Radial velocity (Rv) +3.0[4] km/s
Proper motion (μ) RA: -15.64[1] mas/yr
Dec.: -0.77[1] mas/yr
Parallax (π) 6.23 ± 0.72[1] mas
Distance approx. 520 ly
(approx. 160 pc)
Absolute magnitude (MV) +0.68[5]
Mass 2.47 ± 0.15[5] M
Radius 2.6 ± 0.4[5] R
Luminosity 52[5] L
Surface gravity (log g) 4.01 ± 0.14[5] cgs
Temperature 10,723[6] K
Metallicity [Fe/H] 0.86[6] dex
Rotational velocity (v sin i) 31[7] km/s
Companion GY And B
Period (P) 272.99 days
Semi-major axis (a) > 0.25 AU
Eccentricity (e) 0.47
Argument of periastron (ω)
Other designations
BD +44°341, HD 9996, HIP 7651, HR 465, SAO 37393.[3]
Database references

GY Andromedae (GY And) is an α2 Canum Venaticorum type variable star in the northern constellation Andromeda. Its brightness fluctuates in visual magnitude between 6.27m and 6.41m, making it a challenge to view with the naked eye even in good seeing conditions. The magnetic activity on this star shows an unusually long period of variability, cycling about once every 23 years.[9] Based upon parallax measurements, this star is located at a distance of about 520 light-years (160 parsecs) from the Earth.[1]

This is classified as an Ap/Bp star, with a peculiar spectrum[9] showing lines of chromium and europium that change in intensity over a period matching the variability cycle, although opposite in phase.[10] Its most striking characteristic is the presence of the unstable element promethium in its emission spectrum. All isotopes of this element are radioactive with half lives of 17.7 years or less. The promethium in the outer envelope may be generated by the spontaneous fission of higher mass transuranic elements.[11]

In 1958, American astronomer Horace W. Babcock discovered that this is a spectroscopic binary star. It has an orbital period of 273 days with a large eccentricity of 0.47. The two components are separated by an estimated distance of at least 3.74 × 107 km, or 0.25 Astronomical Units.[8]


  1. ^ a b c d e f van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. Bibcode:2007A&A...474..653V. arXiv:0708.1752Freely accessible. doi:10.1051/0004-6361:20078357. 
  2. ^ a b c Nicolet, B. (1978). "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System". Astronomy and Astrophysics Supplement Series. 34: 1–49. Bibcode:1978A&AS...34....1N. 
  3. ^ a b "V* GY And -- Variable Star of alpha2 CVn type", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-01 
  4. ^ Wilson, R. E. (1953), General Catalogue of Stellar Radial Velocities, Carnegie Institute of Washington, D.C., Bibcode:1953GCRV..C......0W 
  5. ^ a b c d e North, P. (June 1998), "Do SI stars undergo any rotational braking?", Astronomy and Astrophysics, 334: 181–187, Bibcode:1998A&A...334..181N, arXiv:astro-ph/9802286Freely accessible 
  6. ^ a b Aller, M. F. (July 1972), "A model atmosphere analysis of the Ap star HR 465", Astronomy and Astrophysics, 19: 248–260, Bibcode:1972A&A....19..248A 
  7. ^ Royer, F.; et al. (October 2002), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy and Astrophysics, 393: 897–911, Bibcode:2002A&A...393..897R, arXiv:astro-ph/0205255Freely accessible, doi:10.1051/0004-6361:20020943 
  8. ^ a b Scholz, G. (1978), "Spectroscopic investigations of the magnetic AP star HD 9996", Astronomische Nachrichten, 299 (2): 81–85, Bibcode:1978AN....299...81S, doi:10.1002/asna.19782990204 
  9. ^ a b Leroy, J. L. (November 1995), "Linear polarimetry of AP stars. V. A general catalogue of measurements", Astronomy and Astrophysics Supplement, 114: 79, Bibcode:1995A&AS..114...79L 
  10. ^ Preston, George W.; Wolff, Sidney C. (June 1970), "The Very Slow Spectrum, Magnetic, and Photometric Variations of HD 9996", Astrophysical Journal, 160: 1071, Bibcode:1970ApJ...160.1071P, doi:10.1086/150494 
  11. ^ Mitalas, R.; Marlborough, J. M. (April 1973), "Some tests and consequences of the identification of promethium in HR 465", Astrophysical Journal, 181: 475–480, Bibcode:1973ApJ...181..475M, doi:10.1086/152063 

External links[edit]