Angular Momentum Transfer in Dynamically Collapsing Gaseous Disks

Details Angular Momentum Transfer in Dynamically Collapsing Gaseous Disks Angular Momentum Transfer in Dynamically Collapsing Gaseous Disks

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..199n&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

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We investigate the angular momentum transfer in dynamically collapsing disks by using self-similar solutions for self-gravitating viscous disks. As for the mechanisms of angular momentum transfer, the turbulent viscosity and the gravitational torque are considered. We examine the effects of the angular momentum transfer in the disks in the runaway collapse phase, when the central core is not formed yet. As a result, the outward angular momentum transfer makes remarkable differences in rotational velocity distributions comparing with that of the disk with no angular momentum redistribution. On the other hand, the distributions of surface density and infall velocity do not vary significantly, since the effect of the centrifugal force is small in this phase. Also, we find that the angular momentum transfer by gravitational torque tends to work more effectively than that due to turbulent viscosity. This is because the magnitude of effective viscosity of gravitational torque is superior to that of turbulent viscosity if the disk is unstable against self-gravity, which is satisfied in the disks in runaway phase. Lastly we discuss the effects of angular momentum transfer in the disk in runaway collapse phase on the central star, which will be formed in a subsequent star forming phase.

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