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Open Astronomy

formerly Baltic Astronomy

Editor-in-Chief: Barbuy, Beatriz

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IMPACT FACTOR 2017 (Baltic Astronomy): 0.417
5-year IMPACT FACTOR (Baltic Astronomy): 0.486

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Open Access
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ISSN
2543-6376
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Volume 23, Issue 2

Issues

A Tale on Two Close Binaries in Pegasus

H. V. Şenavcı
  • Ankara University, Faculty of Science, Department of Astronomy and Space Sciences, TR-06100, Tandoğan, Ankara, Turkey
  • Other articles by this author:
  • De Gruyter OnlineGoogle Scholar
/ M. Yılmaz
  • Ankara University, Faculty of Science, Department of Astronomy and Space Sciences, TR-06100, Tandoğan, Ankara, Turkey
  • Other articles by this author:
  • De Gruyter OnlineGoogle Scholar
/ Ö. Baştürk / İ. Özavcı
  • Ankara University, Faculty of Science, Department of Astronomy and Space Sciences, TR-06100, Tandoğan, Ankara, Turkey
  • Other articles by this author:
  • De Gruyter OnlineGoogle Scholar
/ Ş. Çalışkan
  • Ankara University, Faculty of Science, Department of Astronomy and Space Sciences, TR-06100, Tandoğan, Ankara, Turkey
  • Other articles by this author:
  • De Gruyter OnlineGoogle Scholar
/ T. Kılıçoğlu
  • Ankara University, Faculty of Science, Department of Astronomy and Space Sciences, TR-06100, Tandoğan, Ankara, Turkey
  • Other articles by this author:
  • De Gruyter OnlineGoogle Scholar
/ C. T. Tezcan
  • Ankara University, Faculty of Science, Department of Astronomy and Space Sciences, TR-06100, Tandoğan, Ankara, Turkey
  • Other articles by this author:
  • De Gruyter OnlineGoogle Scholar
Published Online: 2017-02-18 | DOI: https://doi.org/10.1515/astro-2017-0177

Abstract

We present the simultaneous light and radial velocity curve analysis of two contact binaries in Pegasus using the Wilson-Devinney code. The following absolute astrophysical parameters are determined: masses, radii and effective temperatures. BB Peg is a W-subtype W UMa-type binary, components of which are main sequence stars with 0.50 M and 1.40 M. The radii of its components are R1 = 0.81 R and R2 = 1.28 R. V407 Peg is an A-subtype contact binary composed of two subgiant components with masses 1.70 M and 0.43 M, and radii R1 = 2.17 R and R2 = 1.25 R. Comparisons with the theoretical models for solar composition by Girardi et al. (2000) confirms our classification and supports the results.

Keywords: stars: binaries: eclipsing; stars: fundamental parameters; stars: individual (BB Peg, V407 Peg)

REFERENCES

About the article

Received: 2014-04-29

Accepted: 2014-06-03

Published Online: 2017-02-18

Published in Print: 2014-06-01


Citation Information: Open Astronomy, Volume 23, Issue 2, Pages 123–135, ISSN (Online) 2543-6376, DOI: https://doi.org/10.1515/astro-2017-0177.

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© 2014 H. V. Şenavcı et al., published by De Gruyter Open. This work is licensed under the Creative Commons Attribution-NonCommercial-NoDerivatives 3.0 License. BY-NC-ND 3.0

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