The formation of stars, disks, and planets

我们正在模拟恒星的形成过程，周围的气体和尘埃圆盘，以及凝聚在其中的行星。现在是探索我们起源的令人兴奋的时刻，因为用于模拟的计算能力急剧增加，并且能够与来自新的全球天文台的前所未有的高分辨率和灵敏的地图进行比较。 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。这些质量目前未知的下限对后来的宇宙史有着重要的影响。我们还将从星云坍塌的最早阶段开始，对行星系统(包括气态行星和岩石行星)的形成进行建模。 我们将应用一种新技术，利用尘埃颗粒的极化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这样的断言，即银河系中的磁场可以严重限制恒星的形成速度，并保持星际云中无处不在的湍流运动。

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.