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47 Cygni

From Wikipedia, the free encyclopedia
Star in the constellation Cygnus

47 Cygni

Alight curve for V2125 Cygni, plotted fromHipparcos data[1]
Observation data
Epoch J2000      Equinox J2000
ConstellationCygnus
Right ascension20h 33m 54.18809s[2]
Declination+35° 15′ 03.0390″[2]
Apparent magnitude (V)4.61[3](4.84 + 7.30)[4]
Characteristics
Spectral typeK6: Ib + B2.5:[3]
B−Vcolor index1.593±0.023[5]
Variable typeLc[6]
Astrometry
Radial velocity (Rv)−4.6±0.3[7] km/s
Proper motion (μ)RA: −6.12mas/yr[2]
Dec.: −4.166mas/yr[2]
Parallax (π)0.8792±0.196 mas[2]
Distance4072+965
−773
 ly
(1249+296
−237
 pc)[8]
Absolute magnitude (MV)−4.1(−4 + −1.5)[3]
Orbit[9]
Period (P)1117±11 d
Eccentricity (e)0.00 (assumed)
Periastronepoch (T)2,447,088±10 JD
Semi-amplitude (K1)
(primary)
2.0±0.1 km/s
Details
47 Cyg Aa
Mass12.1±0.2[10]
19.4±3.9[11] M
Radius601[12] R
Surface gravity (log g)1.23[13] cgs
Temperature4,217[13] K
Metallicity[Fe/H]0.13[13] dex
Age17.6±0.6[10] Myr
47 Cyg Ab
Mass0.57[14] M
47 Cyg B
Mass10.96[14] M
Other designations
47 Cyg,V2125 Cyg,BD+34°4079,GC 28630,HD 196093/196094,HIP 101474,HR 7866,SAO 70203,WDS J20339+3515,2MASS J20335419+3515031[15]
Database references
SIMBADdata

47 Cygni is atriple star[4][16] system in the northernconstellation ofCygnus, and is located around4,000 light years from the Earth. It is visible to the naked eye with a combinedapparent visual magnitude of 4.61.[3] The system is moving closer to the Earth with a heliocentricradial velocity of−4.6 km/s.[7]

The dual nature of this system was recognized byAnnie Cannon in 1912, and she assigned the pair separateHenry Draper Catalogue identifiers.[9] They orbit each other with a period of around 143.69 yr.[14] The primary component is itself aspectroscopic binary in a near circular orbit with aperiod of around 3.06 yr. Thea sini value for the primary is 30.8 ± 1.6 Gm (0.206 ± 0.011 AU), wherea is thesemimajor axis andi is theorbital inclination. It has been repeatedly resolved byspeckle interferometery since 1973. Radio emission was detected from this system in 1985/86.[9]

The supergiant primary is aslow irregular variable with an amplitude of about 0.1 magnitudes.[6] Itsangular diameter has been measured at4.472±0.017 milliarcseconds usinginterferometry by theNavy Precision Optical Interferometer.[17] At the distance of 1,249 parsecs,[8] it yield a radius of 601 R.[12] Its close companion has 57% of themass of the Sun.[14] The secondary is a hotB-type main-sequence star, but still 2.5 magnitudes fainter than the primary.[4]

References

[edit]
  1. ^"/ftp/cats/more/HIP/cdroms/cats".Centre de Données astronomiques de Strasbourg. Strasbourg astronomical Data Center. RetrievedOctober 15, 2022.
  2. ^abcdVallenari, A.; et al. (Gaia collaboration) (2023)."Gaia Data Release 3. Summary of the content and survey properties".Astronomy and Astrophysics.674: A1.arXiv:2208.00211.Bibcode:2023A&A...674A...1G.doi:10.1051/0004-6361/202243940.S2CID 244398875. Gaia DR3 record for this source atVizieR.
  3. ^abcdGinestet, N.; Carquillat, J. M. (December 2002)."Spectral Classification of the Hot Components of a Large Sample of Stars with Composite Spectra, and Implication for the Absolute Magnitudes of the Cool Supergiant Components".The Astrophysical Journal Supplement Series.143 (2):513–537.Bibcode:2002ApJS..143..513G.doi:10.1086/342942.
  4. ^abcEggleton, P. P.; Tokovinin, A. A. (September 2008)."A catalogue of multiplicity among bright stellar systems".Monthly Notices of the Royal Astronomical Society.389 (2):869–879.arXiv:0806.2878.Bibcode:2008MNRAS.389..869E.doi:10.1111/j.1365-2966.2008.13596.x.S2CID 14878976.
  5. ^Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation".Astronomy Letters.38 (5): 331.arXiv:1108.4971.Bibcode:2012AstL...38..331A.doi:10.1134/S1063773712050015.S2CID 119257644.
  6. ^abSamus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)".VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S.1.Bibcode:2009yCat....102025S.
  7. ^abGontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system".Astronomy Letters.32 (11):759–771.arXiv:1606.08053.Bibcode:2006AstL...32..759G.doi:10.1134/S1063773706110065.S2CID 119231169.
  8. ^abBailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Demleitner, M.; Andrae, R. (March 1, 2021)."Estimating distances from parallaxes. V: Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3".The Astronomical Journal.161 (3): 147.arXiv:2012.05220.Bibcode:2021AJ....161..147B.doi:10.3847/1538-3881/abd806.ISSN 0004-6256.Gaia eDR3 source for this star.
  9. ^abcGriffin, R. F. (June 1992). "Spectroscopic binary orbits from photoelectric radial velocities. Paper 104: 47 Cygni".The Observatory.112:111–120.Bibcode:1992Obs...112..111G.
  10. ^abTetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (January 2011)."A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun".Monthly Notices of the Royal Astronomical Society.410 (1):190–200.arXiv:1007.4883.Bibcode:2011MNRAS.410..190T.doi:10.1111/j.1365-2966.2010.17434.x.S2CID 118629873.
  11. ^Kervella, Pierre; Arenou, Frédéric; Thévenin, Frédéric (January 1, 2022). "Stellar and substellar companions from Gaia EDR3. Proper-motion anomaly and resolved common proper-motion pairs".Astronomy and Astrophysics.657: A7.arXiv:2109.10912.Bibcode:2022A&A...657A...7K.doi:10.1051/0004-6361/202142146.ISSN 0004-6361.47 Cygni's database entry atVizieR.
  12. ^abLang, Kenneth R. (2006),Astrophysical formulae, Astronomy and astrophysics library, vol. 1 (3 ed.),Birkhäuser,ISBN 3-540-29692-1. The radius (R*) is given by:
    2R=(1031,2494.472) AU0.0046491 AU/R1,201.4R{\displaystyle {\begin{aligned}2\cdot R_{*}&={\frac {(10^{-3}\cdot 1,249\cdot 4.472)\ {\text{AU}}}{0.0046491\ {\text{AU}}/R_{\bigodot }}}\\&1,201.4\cdot R_{\bigodot }\end{aligned}}}
  13. ^abcSoubiran, Caroline; et al. (2016). "The PASTEL catalogue: 2016 version".Astronomy and Astrophysics.591: A118.arXiv:1605.07384.Bibcode:2016A&A...591A.118S.doi:10.1051/0004-6361/201628497.S2CID 119258214.
  14. ^abcdTokovinin, A. (2008)."Comparative statistics and origin of triple and quadruple stars".Monthly Notices of the Royal Astronomical Society.389 (2):925–938.arXiv:0806.3263.Bibcode:2008MNRAS.389..925T.doi:10.1111/j.1365-2966.2008.13613.x.S2CID 16452670.
  15. ^"47 Cyg".SIMBAD.Centre de données astronomiques de Strasbourg. RetrievedJanuary 14, 2019.
  16. ^Mason, Brian D.; et al. (2001)."The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog".The Astronomical Journal.122 (6): 3466.Bibcode:2001AJ....122.3466M.doi:10.1086/323920.
  17. ^Baines, Ellyn K.; Clark III, James H.; Schmitt, Henrique R.; Stone, Jordan M.; von Braun, Kaspar (December 1, 2023)."33 New Stellar Angular Diameters from the NPOI, and Nearly 180 NPOI Diameters as an Ensemble".The Astronomical Journal.166 (6): 268.arXiv:2505.23514.Bibcode:2023AJ....166..268B.doi:10.3847/1538-3881/ad08be.ISSN 0004-6256.
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