SSP seminar

Saving Planetary Cores in MRI-active Disks

Katherine Kretke (Santa Cruz)

Monday 7th December 2009, 12:00pm
Pratt conference room, 60 Garden Street

The hundreds of known planetary systems demonstrate that disk solids are preferentially retained after the dispersal of the original gaseous circumstellar disk. However, in standard protoplanetary disk models, the interactions between the gas and the embedded solids causes the solids to spiral inwards and be lost to the central star on relatively short timescales. In this talk I will discuss how, 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. This scenario presents a robust mechanism to retain solids and may aid in the formation of proto-gas giant cores. Additionally as the structure of protoplanetary disk will influence the orbital evolution of planets we can expect subtle fingerprints of the planet formation process to be present in the observed distribution of planets.


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