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SUMMARY:Three-dimensional simulations of protoplanetary disks with varied 
 thermodynamics\; from gravitational instability to planet migration - Luci
 o Mayer (University of Zurich)
DTSTART:20080526T150000Z
DTEND:20080526T160000Z
UID:TALK11330@talks.cam.ac.uk
CONTACT:Dr. Zoe M. Leinhardt
DESCRIPTION:I will describe the results of state-of-the art 3D simulations
  of\nself-gravitating protoplanetary disks. I will show how\ngravitational
  instability and the eventual direct fragmentation\nof the disk into giant
  planets is strongly dependent on the\nthermodynamics in the disks. The fo
 cus will be on  SPH simulations\nwith flux-limited diffusion. I will then 
 describe the results of a large\ncode comparison for self-gravitating disk
 s which produced the first\nadaptive mesh refinement (AMR) simulations of 
 these systems.\nA novel calculation of possible core formation and envelop
 e enrichment\nin giant planets formed by disk instability will also be pre
 sented.\nFinally\, I will show the first results of new SPH simulations in
  which\nthe 3D interaction between a Jupiter-sized planet and a disk is st
 udied\ntaking into account fully self-consistent dynamics\, self-gravity a
 nd\nradiative transfer. Migration and accretion appear to be both reduced\
 ncompared compared to isothermal simulations\, and the structure of the\nc
 ircumplanetary disk is also affected\, with important implications\nfor th
 e formation of satellites of giant planets.
LOCATION:MR14\, DAMTP\, Pav. F
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