Circumstellar disks are the formation sites of planets, and their physical and chemical characteristics affect the masses and compositions of planets, as well as planet formation timescales and protostellar accretion rates. Millimeter and submillimeter interferometry with instruments like ALMA gives us a detailed look at the gas and dust in disks, particularly dust near the midplane of the disk where planet formation takes place. There is now evidence that planet formation is well under way by the Class II phase of disk evolution, when the envelope has dissipated but a significant amount of gas and dust remains in the disk. Open questions remaining about propoplanetary disk evolution include the sizes of the dust grains in disks and the exact role of the magnetic field in accretion. Through observational studies of polarized emission from protoplanetary disks, I examine the roles of dust grain growth and magnetically-driven protostellar accretion in disk evolution.
Meeting ID: 331 361 9253