Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21534601k&link_type=abstract
American Astronomical Society, AAS Meeting #215, #346.01; Bulletin of the American Astronomical Society, Vol. 42, p.527
Astronomy and Astrophysics
Astronomy
Scientific paper
The radial drift of planetary building-blocks in gas-rich circumstellar disks poses a significant challenge to efficient giant-planet formation. However, both aerodynamic drag and tidal forces, the mechanisms responsible for the drift of meter-sized boulders and earth-mass planetary embryos, respectively, are sensitive to the radial surface density and temperature gradients. Therefore one must accurately calculate the disk structure in order to comment on the motion of solids and the resulting impact on planet formation. In this talk I will demonstrate that in a protoplanetary disk in which angular momentum is transported primarily by MHD turbulence, we expect special locations, planet traps, in which solid material can accumulate. These traps are formed because the angular momentum transport is affected by the thermal structure and the gas-to-dust ratio. As the disk evolves toward a quasi-steady state, radial differences in the effective viscosity will alter the structure of the gas, changing the gas rotation law and altering the both the Lindblad and co-rotation torques. This scenario presents a robust process for the retention of solids that may aid in the formation of proto-gas giant cores. Additionally, by modeling the disk structure we can comment on the processes that influence the orbital distribution of short-period super-earths.
Kretke Katherine A.
Lin Doug N. C.
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