Numerical methods for the simulation of dynamical mass transfer in binaries
We describe computational tools that have been developed to simulate dynamical mass transfer in semidetached, polytropic binaries that are initially executing synchronous rotation upon circular orbits. Initial equilibrium models are generated with a self-consistent field algorithm; models are then evolved in time with a parallel, explicit, Eulerian hydrodynamics code with no assumptions made about the symmetry of the system. Poisson's equation is solved along with the equations of ideal fluid mechanics to allow us to treat the nonlinear tidal distortion of the components in a fully self-consistent manner. We present results from several standard numerical experiments that have been conducted to assess the general viability and validity of our tools, and from benchmark simulations that follow the evolution of two detached systems through five full orbits (up to approximately 90 stellar dynamical times). These benchmark runs allow us to gauge the level of quantitative accuracy with which simulations of semi-detached systems can be performed using presently available computing resources. We find that we should be able to resolve mass transfer at levels M/M > few × 10-5 per orbit through approximately 20 orbits with each orbit taking about 30 hours of computing time on parallel computing platforms.
Publication Source (Journal or Book title)
Astrophysical Journal, Supplement Series
Motl, P., Tohline, J., & Frank, J. (2002). Numerical methods for the simulation of dynamical mass transfer in binaries. Astrophysical Journal, Supplement Series, 138 (1), 121-148. https://doi.org/10.1086/324159