Studies in Stellar Structure and Evolution

我们对恒星演化的理解的物理基础最终是在恒星结构计算模型的成功中测量出来的。首席研究员（PI）将他的职业生涯奉献给了恒星的计算模型，这些模型允许理解恒星如何从“hr图”上的一个位置到另一个位置的时间演变。在过去的三年里，PI开始将他的专业知识扩展到双星的演化，白矮星上富氢物质的吸积及其随后的引力沉降和混合，“慢”中子捕获核合成的随时间计算等难题上。PI新工作的很大一部分将包括吸积和混合的流体动力学模拟。他将继续与藤本先生和他在日本的合作者积极合作，将多维流体动力物理纳入他的模型内部计算机代码中。预计这次联姻将促进日本和美国天文学的理论专业知识。

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.