Later Generations of Light Curve Models

The physical models discussed in this book in greatest detail are those developed by Wilson & Devinney (1971) and later versions by Wilson (1979, 1990, 1998, 2003, 2007). For a brief review of the models we recommend Wilson (1994). Readers interested in the Nelson-Davis-Etzel model should consult Etzel & Leung (1990). Chapter 5 also describes the models and programs by Hill & Rucinski [Hill (1979), Hill & Rucinski (1993)], by Linnell (1984, 1993), by Hadrava (1997, 2004), and others.

The Wilson-Devinney model has been selected as our principal analysis research tool both for its intrinsic virtues and because of its widespread popularity. Its usage has increased to the point that it is used for the majority of light curve analyses performed at the present time (McNally 1991, p. 485), Milone (1993). And last but not least, because it is expandable in the sense that new astrophysical features can be incorporated as the field progresses. Here we mention a few examples: radial velocities (Wilson & Sofia 1976), star spots [Milone et al. (1987), Kang & Wilson (1989)], Kurucz atmospheres (Milone et al. 1992b), line profiles (Mukherjee et al. 1996), radiation pressure effects (Drechsel et al.1995), parameter estimation methods (Kallrath, 1987, 1993), and improvement of convergence by using the Levenberg-Marquardt algorithm (Kallrath et al. 1998).

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