A Computational Guide to Physics of Eclipsing Binaries. I. Demonstrations and Perspectives

By A. Prša, T. Zwitter. 2005

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PHOEBE (PHysics Of Eclipsing BinariEs) is a modeling package for eclipsing binary stars, built on top of the widely used WD program of Wilson & Devinney. This introductory paper gives an overview of the most important scientific extensions (incorporating observational spectra of eclipsing binaries into the solution-seeking process, extracting individual temperatures from observed color indices, main-sequence constraining, and proper treatment of the reddening), numerical innovations (suggested improvements to WD's differential corrections method, the new Nelder & Mead downhill simplex method), and technical aspects (back-end scripter structure, graphical user interface). While PHOEBE retains 100% WD compatibility, its add-ons are a powerful way to enhance WD by encompassing even more physics and solution reliability. The operability of all these extensions is demonstrated on a synthetic main-sequence test binary; applications to real data will be published in follow-up papers. PHOEBE is released under the GNU General Public License, which guarantees it to be free and open to anyone interested in joining in on future development.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/79cbed9af932a4503c105f052f924be60ac6f41f

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Citations in the corpus

Unique sextuple system: 65 Ursae Majoris (2012, methodology): “The LC and RV curves of the eclipsing pair were analyzed using the program PHOEBE (Prša & Zwitter, 2005), which is based on the Wilson-Devinney program (WD, Wilson & Devinney 1971).”
THE MASS–RADIUS(–ROTATION?) RELATION FOR LOW-MASS STARS (2010, methodology): “Several different software packages are commonly used to fit light curves (e.g. Wilson & Devinney 1971; Popper & Etzel 1981; Southworth et al. 2004; Prsa & Zwitter 2005), so it seems possible that the choice of algorithm could be significant.”
NOMINAL VALUES FOR SELECTED SOLAR AND PLANETARY QUANTITIES: IAU 2015 RESOLUTION B3 (2016, methodology): “The eclipsing binary modeling code PHOEBE (Prša & Zwitter 2005, A.Prša et al. 2016, in preparation) has also been updated to use the recommended values.”
KEPLER ECLIPSING BINARY STARS. I. CATALOG AND PRINCIPAL CHARACTERIZATION OF 1879 ECLIPSING BINARIES IN THE FIRST DATA RELEASE (2010, methodology): “The neural network for overcontact EBs is trained on a synthetic sample of 10,000 stars (exemplars) generated by the light curve synthesis code PHOEBE (Prša & Zwitter 2005).”
ON THE USE OF EMPIRICAL BOLOMETRIC CORRECTIONS FOR STARS (2010, background): “(2) One of original coefficients was also misprinted, and a correction was issued by Prša & Zwitter (2005).”
PHYSICS OF ECLIPSING BINARIES. II. TOWARD THE INCREASED MODEL FIDELITY (2016, methodology): “The original PHOEBE model (Prša & Zwitter 2005a) was based on the Wilson–Devinney code (Wilson & Devinney 1971, hereafter WD).”