Protostars and Planets VI, Heidelberg, July 15-20, 2013
TRANSPORT OF SOLID MATERIAL IN DYNAMICALLY EVOLVING 1D DISK MODELS WITH PRESSURE MAXIMA
Tarczay-Nehéz, Dóra (Department of Astronomy, Eötvös Loránd University, Hungary)
Regály, Zsolt (Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Hungary)
Sándor, Zsolt (Department of Astrophysics, University of Vienna, Austria)
Planet formation theory based on the core-accretion scenario suffers from the very fast loss of dust particles, the building blocks of planetesimals. Thus, the available material to build planets is consumed before a significant mass of dust are able to stick together. An effective solution to this problem might be a pressure trap.
The radial drift of the dust particles are caused by the difference in the orbital velocity of the gas and the dust particles. At the edges of the accretionally dead zone in a protoplanetary disk (Gammie, 1996), the gradient of the gas pressure vanishes serving a trap for dust particles under inward drift. The increased density of dust particles there may accelerate the formation of planetesimals, and by subsequent collisions even the formation of planets and planetary cores.
In the present work we investigate the mass growth due to the dust particle accumulation in pressure maxima. Our results support the idea of rapid planet formation via core-accretion, but we find that the efficiency of dust accumulation depends on the disk physical parameters.
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