THE FORMATION OF PROTOSTELLAR DISKS .2. DISKS AROUND INTERMEDIATE-MASS STARS

Hydrodynamical calculations of the evolution of a collapsing, rotating axisymmetric 10 M. molecular clump, including the effects of radiative acceleration but without magnetic fields, are presented. The initial cloud is assumed to be a uniformly rotating, centrally condensed sphere with rho proportional to r(-2). Several cases are considered, in which both the overall clump size and the total amount of angular momentum are varied. The calculations show how a warm, quasi-hydrostatic disk surrounding a central unresolved core of only a few solar masses forms and grows in size and mass. The disk is encased in two distinct accretion shock fronts, both of which are several scale heights above the equatorial plane. At the end of the calculation of our standard case, the central unresolved region is found to have a mass of 2.7 M. and a ratio of rotational to gravitational energy of similar to 0.45, sufficiently large to be unstable to nonaxisymmetric perturbations. In addition, the inner portions of the disk containing most of the mass are unstable according to the local Toomre criterion, implying that also in this region nonaxisymmetric perturbations will lead to rapid evolution. Under the assumption that gravitational torques would transport angular momentum out of this region, a central core of less than or similar to 8 M. with a stable disk of greater than or similar to 2 M. should result. Frequency-dependent radiative transfer calculations of the standard case at selected ages show how the continuum spectrum of the structure depends on the disk's orientation and age and how the observed isophotal contours vary with wavelength. Because of the strong dependence on viewing angle, continuum spectra alone should not be used to estimate the evolutionary stage of development of these objects. Comparable results were obtained for the other cases considered.