The formation of stars, disks, and planets

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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.