The physical basis for our understanding of the stellar evolutionary is ultimately measured in the success of computational models of stellar structure. The Principal Investigator (PI) has devoted his career to computing models of stars that permit an understanding of how stars evolve in time from one position on the "H R Diagram" to another. In the last three years the PI has begun to extend his expertise to the difficult problems of the evolution of binary stars, the accretion of hydrogen-rich material onto white dwarfs and its subsequent gravitational settling and mixing, time- dependent computations of "slow" neutron-capture nucleosynthesis. A substantial part of the PI's new work will include hydrodynamical simulations of accretion and mixing. He will continue a vigorous collaboration with M. Fujimoto and his collaborators in Japan to include multi-dimensional hydrodynamical physics into his model interior computer codes. It is anticipated that this marriage will facilitate added theoretical expertise to both Japanese and U.S. astronomy.
