Theoretical Studies in Interstellar Astrophysics

星际气体聚集成恒星的过程是 天体物理学中的基本问题， 星系的形成和演化以及 元素 分子云的结构和演化 银河系星星形成的地点，将由Dr。 麦基 分子云被观察到高度聚集， 计算将确定介质之间的性质 成团 分子云的早期演化， 大部分原子气体变成分子，将被计算。 的 重力束缚的团块中的压力分布 研究了 计算会追踪到 巨大的恒星形成的星云。 冲击波 塑造弥漫的星际云的质谱， 强大的流体动力学和磁流体动力学计算机代码将 用于研究激波与云的相互作用。 休克 波可以产生水脉泽，这是大质量星星的路标 形成，而这种情况可能发生的条件将是 评估。 星际介质中的许多重元素， 由恒星产生的尘埃，被锁在微小的尘埃颗粒中， 溅射，蒸发，粉碎这些颗粒， 将计算星际冲击。

The process by which interstellar gas gathers into stars is a fundamental problem in astrophysics, with implications for the formation and evolution of galaxies and the formation of the elements. The structure and evolution of molecular clouds, the sites of Galactic star formation, will be investigated by Dr. McKee. Molecular clouds are observed to be highly clumped, and calculations will determine the nature of the medium between the clumps. The early evolution of a molecular cloud, in which a largely atomic gas becomes molecular, will be calculated. The distribution of pressure in gravitationally bound clumps will be investigated. Calculations will trace the destruction of the clouds by the massive stars that form within them. Shock waves shape the mass spectrum of diffuse interstellar clouds, and powerful hydrodynamic and magnetohydrodynamic computer codes will be used to study the interaction of shocks with clouds. Shock waves can produce water masers, which are signposts of massive star formation, and the conditions under which this can occur will be evaluated. Many of the heavy elements of the interstellar medium, which are produced by stars, are locked up in tiny dust grains; the sputtering, vaporization, and shattering of these grains in interstellar shocks will be calculated.