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SUMMARY:Dust dynamics in self-gravitating disks – could planet formation
  start in young disks?
DTSTART;VALUE=DATE-TIME:20200514T144500Z
DTEND;VALUE=DATE-TIME:20200514T150500Z
DTSTAMP;VALUE=DATE-TIME:20240704T115620Z
UID:indico-contribution-70@meetings.aip.de
DESCRIPTION:Speakers: George Mamatsashvili (Helmholtz-Zentrum Dresden-Ross
 endorf)\nI will present the results on the evolution of dust particles in 
 self-gravitating disks residing in a gravitoturbulent state\, when heating
  due to shocks of density waves balances cooling.  It is well known that d
 ensity structures in the gaseous component of the disk induced by self-gra
 vity (gravitational instability) can trap dust efficiently enough\, so tha
 t the dust component itself undergoes further gravitational collapse due t
 o its own self-gravity. Previous results both in global and local shearing
  box studies indicate that over-pressure regions related to spiral density
  waves can be very efficient at collecting dust particles\, creating signi
 ficant local over-densities of particles. The degree of such concentration
 s depends on two parameters: the size of dust particles and the rate of ga
 s cooling. In recent years\, increasing observational evidence indicates t
 hat large-scale vortices (e.g.\, induced by planetary gaps) and rings are 
 most preferable sites of dust trapping. \n\nMotivated by this\, we studied
  effects of vortices on the evolution of dust particles using local sheari
 ng box simulations of self-gravitating protoplanetary disks\, including al
 so the dust-back reaction on gas and self-gravity of the dust component it
 self. In contrast to non-self-gravitating disks\, vortices in self-gravita
 ting disks tend to be smaller-scale (of the order of local Jeans scale) an
 d short-lived structures. We found that these types of structures are neve
 rtheless quite efficient at trapping small and intermediate-sized dust par
 ticles with friction times comparable to\, or less than\, the local orbita
 l period of the disk. This can lead to significant over-densities in the s
 olid component of the disk\, with density enhancements comparable to\, and
  even higher\, than those within spiral density waves\; increasing the rat
 e of gravitational collapse of dust into bound structures (planetesimals).
  I will also discuss the resulting surface density structure of dust trapp
 ed in such vortices in connection with recent observations of disks.\n\nht
 tps://meetings.aip.de/event/1/contributions/70/
LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall
URL:https://meetings.aip.de/event/1/contributions/70/
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