Mapping Protostellar Magnetic Fields from Cores to Disks

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The star formation rate in the Milky Way is extremely inefficient, with only ~1-10% of the available gas being converted to stars. This is due to turbulence, magnetic fields, and stellar feedback playing important roles in this process. Arguably, magnetic fields remain the least understood of these. Simulations have shown magnetic fields can control when a protostar forms a disk. Observational studies of cloud cores down to disks have attempted to look for morphology changes in this critical region, yet have mostly lacked proper spatial coverage to statistically determine how, or if, this occurs. In this talk, I will go over the current status of magnetic field observations in young disks, and discuss how CMB-S4 observations will help to answer key questions in star formation.