The formation of stars, disks, and planets

我们正在模拟恒星的形成过程，周围的气体和尘埃盘，以及在其中凝聚的行星。这是一个探索我们起源的激动人心的时刻，因为模拟计算能力的急剧增加，以及与来自新的全球天文台的前所未有的高分辨率和敏感地图进行比较的能力。 我们将使用我们的盘形成和演化计算机模拟代码来确定可能在早期宇宙中形成的恒星的质量。目前未知的这些质量的下限对随后的宇宙历史有着重要的影响。我们还将模拟行星系统（包括气态和岩石行星）的形成，从星云云坍缩的最早阶段开始。 我们将采用一种新技术，利用尘埃颗粒的偏振电磁辐射数据来确定星际云中的磁场强度。我们还将应用我们自己的计算机模拟代码来测试银河系中的磁场可以严重限制恒星形成的速度，并且还可以维持星际云中普遍观察到的湍流运动。

We are modeling the formation process of stars, surrounding disks of gas and dust, and the planets that condense within them. This is an exciting time to be exploring our origins, due to dramatic increases in computational power for simulations, and the ability to compare with unprecedented high-resolution and sensitive maps from new global observatories. We will employ our disk formation and evolution computer simulation code to determine the masses of stars that could form in the early universe. The presently unknown lower limit to these masses has important consequences for subsequent cosmic history. We will also model the formation of planetary systems (including both gaseous and rocky planets) starting from the earliest stages of collapse of a nebular cloud. We will apply a new technique to determining the strength of magnetic fields in interstellar clouds using data of polarized electromagnetic emission from dust grains. We will also apply our own computer simulation code to test the assertion that magnetic fields in the Galaxy can severely limit the rate at which stars form, and also maintain the ubiquitously observed turbulent motions in interstellar clouds.