Short-Period Binary Star Modeling: The Tools of the Trade and the Products they Produce

Details Short-Period Binary Star Modeling: The Tools of the Trade and the Products they Produce Short-Period Binary Star Modeling: The Tools of the Trade and the Products they Produce

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.4001m&link_type=abstract

American Astronomical Society Meeting 208, #40.01; Bulletin of the American Astronomical Society, Vol. 38, p.114

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The purpose of this section of the Short-Period Binary session is to report on results from systems less evolved than black-holes, neutron stars, and white dwarfs, and in doing this to emphasize the modeling techniques that have been developed to date and those on the horizon. Some of our suggestions for future development (and, in fact, in current development) may allow the tools to be used for systems with more evolved components.In this review, we discuss the available analytic techniques for light curve modeling, such as simplex, damped least squares, auto-iterative adjustment, and simultaneous light and RV curve modeling, use of polarimetric and color index data, spot modeling, modeling of translucent clouds in stellar atmospheres, and the full parameter adjustment capability currently available in versions of the Wilson-Devinney program. We also discuss such metaheuristics (which are non-problem specific) as synthetic annealing and genetic algorithms. We describe the results of applications of the techniques to eclipsing binaries across a range of contact configurations and evolutionary states, including binaries in clusters.Additionally, we suggest tasks for inclusion in the next generation modeling code, some of which are carried out in excellent but separate programs. A few are: Stellar tomography; Zeeman Doppler image modeling of magnetic field structures in interacting binaries; and the incorporation of a wider range of atmospheric models (in T and log g grids) than is currently available in most light curve modeling codes, for more adequate modeling of: (a) binary systems with greatly disparate components, such as white dwarfs and red or even brown dwarfs or planets; (b) the narrow neck region of overcontact systems; and (c) low temperature starspots on stars with active regions.This work is being supported in part by Canadian NSERC grants to EFM.

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