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Physics of Eclipsing Binaries: Motivation for the New-Age Modeling Suite

Published online by Cambridge University Press:  25 February 2014

A. Prša ,
P. Degroote ,
K. Conroy ,
S. Bloemen ,
K. Hambleton ,
J. Giammarco  and
H. Pablo
A. Prša
Affiliation:
Dept. of Astrophysics and Planetary Science, Villanova University, 800 Lancaster Ave., Villanova, PA 19085, USA
P. Degroote
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
K. Conroy
Affiliation:
Department of Physics and Astronomy, Vanderbilt University, VU Station B 1807, Nashville, TN 37235, USA
S. Bloemen
Affiliation:
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
K. Hambleton
Affiliation:
Jeremiah Horrocks Institute, University of Central Lancashire, Preston, PR1 2HE, UK
J. Giammarco
Affiliation:
Department of Astronomy and Physics, Eastern University, Saint Davids, PA 19087, USA
H. Pablo
Affiliation:
Département de Physique, Université de Montréal, CP 6128, Succursale Centre-Ville, Montréal, QC, H3C 3J7, Canada
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Abstract

Modeling tools for eclipsing binary stars are lagging behind the modern observations that are unprecedented both in quality and in quantity. We assembled a team of modeling and interpretation experts and propose to enhance the modeling code to tackle this new-age data. In this paper we outline some of the most important advancements planned and being implemented into the new version of the phoebe code. These advancements will greatly reduce systematics and allow us to focus on prime astrophysics to be gleaned in studying eclipsing binaries and exoplanet transits. For the first time the errors on the masses and radii will be pushed well below 1%.

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