A General Approach to Modeling Eclipsing Binaries

  • Josef Kallrath
  • Eugene F. Milone


This chapter provides the basis to compute observables for a given set of eclipsing binary parameters and a given set of times or phases. Typical observables are light curves, radial velocity curves, polarization curves, and line profiles. Since in this chapter the focus is on general considerations, no details of implementation are given. Those are found in Chapter 5 for several light curve models.1 Eclipsing binary data analysis leads to a nonlinear least-squares problem in which observed curves are compared with model curves. The presentation is greatly simplified if we take the following formal approach: we formally define an eclipsing binary observable curve, Ο, as a mathematical object
$$ O: = \left\{ {\left( {{t_{k,}}{O_k}} \right)\left| {1 \leqslant k \leqslant n} \right.} \right\} $$
,i. e., as a set of n elements in which each element is a pair, (t, o), where t represents an independent, time-related quantity and o is the corresponding observable. The quantity t used as the independent quantity may either represent:
  • time; or

  • the photometric phase ɸ defined in formula (2.1.1).


Light Curve Circular Orbit Radiation Pressure Surface Brightness Binary Star 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


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Copyright information

© Springer Science+Business Media New York 1999

Authors and Affiliations

  • Josef Kallrath
    • 1
    • 2
  • Eugene F. Milone
    • 3
  1. 1.BASF-AGLudwigshafenGermany
  2. 2.Department of AstronomyUniversity of FloridaGainesvilleUSA
  3. 3.Department of Physics and AstronomyUniversity of CalgaryCalgaryCanada

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