Conveners
Thursday Afternoon
- Hubert Klahr (MPIA)
Philip Armitage
(University of Colorado)
07/08/2014, 14:00
Workshop Main Programme
Simple dynamical models for planet formation start from initial conditions in which planetesimals form across a broad range of radii in a smooth gas disk. Such conditions are hard to reconcile with current thinking, which emphasizes the primacy of aerodynamic drift, dead zones, and planetesimal formation via the streaming instability. I will discuss the possibility that most planet formation...
Dr
Steve Desch
(Arizona State University)
07/08/2014, 14:30
Workshop Main Programme
The magnetorotational instability (MRI) is predicted to occur in the more ionizaed regions of protoplanetary disks (PPDs), but it is recognized that the MRI cannot act in magnetically “dead”, less ionized zones (Jin et al. 1996; Gammie 1996; Sano et al. 2002, etc.). As the actions of Ohmic dissipation, ambipolar diffusion and Hall effects have become better understood, doubts have been raised...
Troels Haugbølle
(NBI & StarPlan)
07/08/2014, 15:30
Workshop Main Programme
We use the adaptive mesh refinement computer code RAMSES to model, for the first time, the formation of protoplanetary disks in realistic star formation environments, with resolution scaling over a billion, covering a range from outer scales of about 50 pc to inner scales of less than 0.01 AU. The models are done in three steps, with the first step having a dynamic resolution of ~65,000,...
Prof.
Åke Nordlund
(Niels Bohr Institute & StarPlan)
07/08/2014, 16:00
Workshop Main Programme
The Standard Accretion Disk (SAD) model, based on the assumption that angular momentum transport in accretion disk is mainly in the radial direction, has been the at the center of much of the work on accretion disks since the days of Lynden-Bell & Pringle (1974) and Shakura & Sunyaev (1976). Remarkably, over essentially the same period of time, a completely different – and most likely much...
