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Hi-fi phenomenological description of eclipsing binary light variations as the basis for their period analysis

Published online by Cambridge University Press:  25 February 2014

Z. Mikulášek ,
M. Zejda ,
M. Chrastina ,
S.-B. Qian  and
L.-Y. Zhu
Z. Mikulášek
Affiliation:
Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic Observatory & Planetarium of J. Palisa, VŠB–Technical University, Ostrava, Czech Republic
M. Zejda
Affiliation:
Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic
M. Chrastina
Affiliation:
Department of Theoretical Physics and Astrophysics, Masaryk University, Brno, Czech Republic
S.-B. Qian
Affiliation:
National Astronomical Observatories/Yunnan Observatory of Chinese Academy of Sciences, Kunming, China Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, China
L.-Y. Zhu
Affiliation:
National Astronomical Observatories/Yunnan Observatory of Chinese Academy of Sciences, Kunming, China
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Abstract

In-depth analysis of eclipsing binary (EB) observational data collected for several decades can inform us about a lot of astrophysically interesting processes taking place in the systems. We have developed a wide-ranging method for the phenomenological modelling of eclipsing binary phase curves that enables us to combine even very disparate sources of phase information. This approach is appropriate for the processing of both standard photometric series of eclipses and data from photometric surveys of all kind. We conclude that mid-eclipse times, determined using the latest version of our “hi-fi” phenomenological light curve models, as well as their accuracy, are nearly the same as the values obtained using much more complex standard physical EB models.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 64: Setting a New Standard in the Analysis of Binary Stars , 2013 , pp. 299 - 302
Copyright
© EAS, EDP Sciences, 2014

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References

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