3D Hydrodynamics and Radiative Transfer
Finite difference codes for the solution of the fully three dimensional equations of hydrodynamics, self-gravitation, and radiative transfer have been developed for use on relatively modest computers. Originally developed to study the collapse and fragmentation of protostellar clouds, this family of codes has been used to study a variety of astrophysical problems, with a particular emphasis on cosmogonical issues.
KeywordsRadiative Transfer Diffusion Approximation Solar Nebula Specific Internal Energy Astrophysical Problem
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