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P. M. Motl, J. Frank, J. E. Tohline (Louisiana State University)
We will present results from three-dimensional numerical simulations of dynamical mass transfer in near contact binaries. The binary components are assumed to be polytropic fluid bodies that are initially synchronously rotating. The gravitational and centrifugal potentials are calculated self-consistently for both the initial state and during the hydrodynamic evolution. In particular we will compare the boundary for onset of mass transfer instability in the fully nonlinear hydrodynamic regime with linearized analytic predictions. We will also present a technique for modeling the mass radius relation and the adiabatic radial response to mass loss for main sequence stars with both convective and radiative envelopes as polytropic fluids with nonuniform entropy distributions.
The author(s) of this abstract have provided an email address for comments about the abstract: motl@rouge.phys.lsu.edu