Star Formation in Galaxies

天文学研究的一个主要课题是恒星 是由星际气体的引力坍缩形成的 云 主要研究者（PI）希望提前 由NSF支持的研究，对原核生物的数值模拟， 星星在引力和自转的相互影响下。 的PI 将使用复杂的新数值技术来计算模型 在二维和三维空间中。 模型将被计算为“遵循” 这种崩溃的时间，特别注意的发展， 微小的密度波动最终会变成 行星或二级星星。 NSF的支持将包括购买 这样模拟坍塌的电影 在广泛的测试条件下“真实的时间”进行跟踪。 这些结果有望增加我们对如何 原恒星在坍缩过程中会失去角动量， 定义导致形成两个独立的 “双星”

A major topic of study in astronomy concerns the way in which stars are formed from the gravitational collapse of interstellar gas clouds. The Principal Investigator (PI) wishes to extend earlier studies supported by the NSF of numerical simulations of proto- star under the mutual influence of gravity and rotation. The PI will use sophisticated new numerical techniques to compute models in two and three dimensions. Models will be computed to "follow" this collapse in time, with particular attention to the development of minor density fluctuations which could grow ultimately into planets or a secondary star. NSF support will include the purchase of a computer workstation so that movies of simulated collapses can be followed in "real time" over a wide range of test conditions. These results are expected to increase our understanding of how proto-stars lose angular momentum during their collapse and to define the conditions leading to the formation of two separate "binary" stars.