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SUMMARY:The formation of high density dust rings and clumps: the role of v
 orticity - Clement Surville  (University of Zurich)
DTSTART:20180212T140000Z
DTEND:20180212T150000Z
UID:TALK96979@talks.cam.ac.uk
CONTACT:Dr. Yufeng Lin
DESCRIPTION:The dust contain of young protoplanetary disks is of crucial i
 nterest.\nAs a building material for pebbles\, planetesimals\, and planeta
 ry cores\, dust is at the heart of planet formation scenarios.\nThe increa
 sing number of observations of young disks in the sub-millimeter wavelengt
 h or in scattered light reveals also many structures in the dust distribut
 ion\, like asymmetries\, gaps and bumps.\nExplaining these observations as
  well as and their confrontation with theoritical models drive a lot of ef
 forts to improve the numerical models of disk evolution and dynamics.\nTha
 nks to several years of experience in multi-fluid simulations of these dus
 ty protoplanetary disks\, I will present new updates about how dust concen
 trations can rise due to the vorticity of the gas.\nWhen large scale vorti
 ces form because of different instabilities\, they tend to accumulate dust
 \, even very small grains\, and change dramatically the distribution of so
 lids on long timescales.\nSuper Earth planets also generate zonal flows\, 
 and even a gap in the disk\, which also trigger dust concentrations in the
  form of disk-wide rings\, with dust-to-gas ratios above unity.\nI will sh
 ow the details and the possibilities of this scenario\, and its implicatio
 ns as a new path bridging different instabilities necessary for a robust p
 lanet formation model.\n
LOCATION:MR14\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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