Statistics – Computation
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dda....40.0501c&link_type=abstract
American Astronomical Society, DDA meeting #40, #5.01; Bulletin of the American Astronomical Society, Vol. 41, p.898
Statistics
Computation
Scientific paper
Planet formation takes place against a backdrop of an evolving protoplanetary disk. The dynamics of dust grains, disk chemistry, the formation of planetesimals, planetary growth, and planetary migration all depend on the surface density and temperature within the disk. Here, I will describe a new analytic model that gives the midplane temperature and surface density in a protoplanetary disk at any point in space and time. A typical disk consists of three regions. In the inner disk, the temperature is mainly determined by energy released as a result of the disk's viscous evolution. In the outer disk, stellar irradiation is the dominant heat source. Close to the star, viscous heating is dominant, but the opacity declines rapidly with increasing temperature as dust grains sublimate. Changes in the protostellar radius and temperature over time can also be incorporated into the model. The model is specifically designed for use in simulations of planetary formation, providing a self-consistent model for the evolution of the disk at minimal computational cost.
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