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Most analytic work to date on protostellar disks has focused on those inisolation from their environments. However, observations are now beginning toprobe the earliest, most embedded phases of star formation, during which disksare rapidly accreting from their parent cores and cannot be modeled inisolation. We present a simple, one-zone model of protostellar accretion diskswith high mass infall rates. Our model combines a self-consistent calculationof disk temperatures with an approximate treatment of angular momentumtransport via two mechanisms. We use this model to survey the properties ofprotostellar disks across a wide range of stellar masses and evolutionarytimes, and make predictions for disks' masses, sizes, spiral structure, andfragmentation that will be directly testable by future large-scale surveys ofdeeply embedded disks. We define a dimensionless accretion-rotation parameterwhich, in conjunction with the disk's temperature, controls the disk evolution.We track the dominant mode of angular momentum transport, and demonstrate thatfor stars with final masses greater than roughly one solar mass, gravitationalinstabilities are the most important mechanism as most of the mass accumulates.We predict that binary formation through disk fission, fragmentation of thedisk into small objects, and spiral arm strength all increase in importance tohigher stellar masses.

Global Models for the Evolution of Embedded, Accreting Protostellar Disks