Prof. Ilaria Pascucci
University of Arizona
Angular Momentum Transport in Protoplanetary Disks: Re-distribute or extract, that is the question
It is well established that young stars accrete disk gas, yet the physical mechanism that enables gas to lose angular momentum, hence accrete onto the star, is still hotly debated. I will discuss how recent disk mass measurements, mass accretion rates, and disk wind diagnostics constrain the two main modes of angular momentum transport in disks, i.e. magneto-rotational instability which re-distributes angular momentum within the disk and magnetohydrodynamic disk winds which extract angular momentum from the disk. I will point out how these different modes affect planetesimal and planet formation and examine which data are required to establish which of the two is the main driver of disk evolution.
Location: 31 Fitzwilliam Place, D02 XF86