Theoretical Studies in Interstellar Astrophysics

星际介质在中小尺度上的动力学 尺度的大小取决于恒星的能量注入， 特别是电离辐射风和超新星 大质量恒星的爆炸 电离氢的演化 区域，无论是孤立的大质量恒星和集群， 在不均匀介质中的恒星将由麦基博士进行研究。 的 超新星爆炸残余物的动力学和光谱 在电离氢区将计算，和 评估了对所观察到的残留物统计数据的影响。 来自大质量恒星群的超新星产生了一个“超级气泡” 在星际介质中;这种结构的动力学将 接受调查，并应用于银河系和 星暴星系 一个强大的新的流体力学计算机代码 将被用来解决一些基本的问题，在星际 能量注入引起的气体动力学，包括相互作用 冲击波与星际云的碰撞 的光谱 星际冲击为天文学家提供了重要的诊断 研究恒星能量注入效应的工具，以及 对分子气体中激波结构的全面研究 已经计划好了 广泛的计算将发展出这一假说 星际水脉泽是由于密集分子的冲击 气体 恒星通过辐射为星际介质提供能量， 恒星在星星的一生中， 超新星在死亡时爆炸。 这种能量最终 辐射到星系际空间，所以 星际介质可以看作是一种能量流， 起源于恒星的几种形式，通过 星际介质，最后离开银河系的形式， 辐射宇宙射线极端情况下还有风 之一 星际天体物理学的中心问题是了解如何 恒星能量注入产生的物理条件， 星际介质的形态，无论是在我们的银河系， 其他星系 麦基博士的研究将集中在能源 大质量恒星的能量注入， 进入星际介质。

The dynamics of the interstellar medium on small and intermediate scale sizes is governed by energy injection from stars, particularly the ionizing radiation, winds, and supernova explosions of massive stars. The evolution of ionized hydrogen regions, both around isolated massive stars and clusters of such stars, in an inhomogeneous medium will examined by Dr. McKee. The dynamics and spectra of the remnants of supernovae which explode in ionized hydrogen regions will be calculated, and the implications for the observed statistics of remnants assessed. Supernovae from a cluster of massive stars create a "superbubble" in the interstellar medium; the dynamics of such structures will be investigated, with applications both to the Galaxy and to starburst galaxies. A powerful new hydrodynamics computer code will be used to address some fundamental problems in interstellar gas dynamics posed by energy injection, including the interaction of a blast wave with an interstellar cloud. The spectra of interstellar shocks provide astronomers with essential diagnostic tools for the study of the effects of stellar energy injection, and a comprehensive attack on the structure of shocks in molecular gas is planned. Extensive calculations will develop the hypothesis that interstellar water masers are due to shocks in dense molecular gas. Stars energize the interstellar medium through radiation and stellar wiinds during the star's life, and for some stars, through supernova explosions at their death. This energy is eventually radiated into intergalactic space, so the energization of the interstellar medium may be viewed as an energy flow which originates in stars in several forms, streams outward through the interstellar medium, and finally leaves the Galaxy in the form of radiation, cosmic rays, and in extreme cases, a wind. One of the central problems in interstellar astrophysics is to understand how stellar energy injection produces the physical conditions and morphology of the interstellar medium, both in our Galaxy and in other galaxies. Dr. McKee's research will focus on energy injection by massive stars, which dominates the energy injection into the interstellar medium.