Conveners
Friday Morning
- Shu-ichiro Inutsuka (Nagoya University)
Prof.
James Stone
(Princeton University)
08/08/2014, 09:00
Workshop Main Programme
The interaction of a planet with a viscous hydrodynamic disk has been well studied in the literature. However, protoplanetary disks are not viscous hydrodynamical flows. Rather, they are inviscid (in the dead zone), or they are turbulent (where the magnetic field couples to the gas). We present some recent studies of the interaction of low-mass planets with both inviscid hydrodynamical...
Dr
Zhaohuan Zhu
(Princeton University)
08/08/2014, 09:30
Workshop Main Programme
Turbulence in protoplanetary disks affects various stages of planet formation. First, it prevents particles' settling to the disk midplane, making planetesimal formation more difficult. Second, it causes stochastic planet migration and prevents gap opening by planets. By carrying out global MHD simulations with dust particles, we have studied settling and radial drift of dust particles in MRI...
Dr
Chao-Chin Yang
(Lund University)
08/08/2014, 10:30
Workshop Main Programme
The streaming instability is a promising mechanism to overcome the barriers in direct dust growth and lead to the formation of planetesimals. Most previous studies of the streaming instability, however, were focused on a local region of a protoplanetary disk with a limited simulation domain such that only one filamentary concentration of solids has been observed. The characteristic...
Dr
Anders Johansen
(Lund University)
08/08/2014, 11:00
Workshop Main Programme
Dust sedimentation is controlled by the strength of the gas turbulence. The degree of sedimentation is one of the most important factors in setting the conditions for planetesimal formation and pebble accretion. I will present a self-consistent theory framework for planet formation, from dust to fully-fledged planets, and highlight phases in the growth where progress requires an increased...
