Abstract
The Wilson–Devinney model has—over the last 50 years—become the standard in analyzing eclipsing binary observations. To provide orientation for both active binary and non-binary researchers, it is presented here in historical and on-going as well as astrophysical perspectives. Among the important advances that originated with the model are: the representation of star surfaces as equipotentials for circular and eccentric orbits, leading to four morphological types; simultaneous least-squares light and velocity curve analyses; efficient reflection computation, including multiple reflection; disk theory and disk modeling. Solutions in physical units allowed for the accurate estimation of parameters such as stellar masses and photometric distances; inclusion of types of observables, properly weighted.
Highlights
Publisher’s Note: MDPI stays neutral with regard to jurisdictional claims in Binary stars, especially eclipsing binaries (EBs),1 provide rich data of various kinds
As readers may be active binary and non-binary researchers, the second group may want to start with the orientation in the Appendix A or enjoy the publication by Wilson [1], which covers the basics of light curve analysis fairly extensively, and return to this point
We focus mainly on modeling ideas and principles rather than the WD computer program that is based on the Wilson–Devinney model (WDM)
Summary
Embedding Roche geometry appropriately into the model and program, leads to an important example of improved astrophysical understanding through EB light curve analysis: The successful modeling of W UMa stars as over-contact systems. These very abundant binaries are excellent laboratories for convection in stars. To readers outside the EB community, the nomenclature may require some caution when it comes to primary and secondary stars Another surprise could be that most (Eclipsing) Binary models and programs nowadays do not use radii as adjustable parameters but rather the Roche potentials Ω1 and Ω2 , which cover the full range of morphological types from detached and semi-detached to over-contact binaries.
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