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GY Andromedae

From Wikipedia, the free encyclopedia
Variable star in the constellation Andromeda
GY Andromedae

Avisual bandlight curve for GY Andromedae, adapted from Metlovaet al. (2014)[1]
Observation data
Epoch J2000      Equinox J2000
ConstellationAndromeda
Right ascension01h 38m 31.82552s[2]
Declination+45° 23′ 58.9357″[2]
Apparent magnitude (V)6.36[3]
Characteristics
Spectral typeB9 pe[4]
U−Bcolor index-0.10[3]
B−Vcolor index+0.04[3]
Variable typeα2 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]
Distance460 ± 10 ly
(141 ± 3 pc)
Absolute magnitude (MV)+0.68[6]
Details
Mass2.47 ± 0.15[6] M
Radius2.6 ± 0.4[6] R
Luminosity52[6] L
Surface gravity (log g)4.01 ± 0.14[6] cgs
Temperature10,723[7] K
Metallicity[Fe/H]0.86[7] dex
Rotational velocity (v sin i)31[8] km/s
Orbit[9]
CompanionGY 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
SIMBADdata

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]

System

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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]

References

[edit]
  1. ^Metlova, N. V.; Bychkov, V. D.; Bychkova, L. V.; Madej, J. (23 August 2014)."Photometric and Magnetic Variability of the Ap Star GY And".Astrophysical Bulletin.69 (3):315–320.Bibcode:2014AstBu..69..315M.doi:10.1134/S1990341314030067. Retrieved25 August 2024.
  2. ^abcdefBrown, A. G. A.; et al. (Gaia collaboration) (2021)."Gaia Early Data Release 3: Summary of the contents and survey properties".Astronomy & Astrophysics.649: A1.arXiv:2012.01533.Bibcode:2021A&A...649A...1G.doi:10.1051/0004-6361/202039657.S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source atVizieR.
  3. ^abcNicolet, 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.
  4. ^ab"V* GY And -- Variable Star of alpha2 CVn type",SIMBAD,Centre de Données astronomiques de Strasbourg, retrieved2012-01-01
  5. ^Wilson, R. E. (1953), "General Catalogue of Stellar Radial Velocities",Carnegie Institute Washington D.C. Publication, Carnegie Institute of Washington, D.C.,Bibcode:1953GCRV..C......0W
  6. ^abcdeNorth, P. (June 1998), "Do SI stars undergo any rotational braking?",Astronomy and Astrophysics,334:181–187,arXiv:astro-ph/9802286,Bibcode:1998A&A...334..181N
  7. ^abAller, 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
  8. ^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,arXiv:astro-ph/0205255,Bibcode:2002A&A...393..897R,doi:10.1051/0004-6361:20020943,S2CID 14070763
  9. ^abScholz, 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
  10. ^abLeroy, 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
  11. ^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
  12. ^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
  13. ^Harper, W. E. (1937)."The radial velocities of 917 stars".Publications of the Dominion Astrophysical Observatory Victoria B.C.7:1–97.Bibcode:1937PDAO....7....1H.
  14. ^Babcock, Horace W. (1958)."A Catalog of Magnetic Stars".Astrophysical Journal Supplement.3:141–210.Bibcode:1958ApJS....3..141B.doi:10.1086/190035.

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