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SUMMARY:Planetesimal formation in gravito-turbulent discs  - Richard Booth
  (IoA)
DTSTART:20170214T130000Z
DTEND:20170214T140000Z
UID:TALK70549@talks.cam.ac.uk
CONTACT:Jean Teyssandier
DESCRIPTION:How km-sized planetesimals are formed from dust grains remains
  a mystery\, with many barriers to growth preventing growth by coagulation
  beyond mm-sizes. For this reason\, collective mechanisms that concentrate
  dust grains sufficiently to allow gravitational collapse to jump the inte
 rmediate sizes and form planetesimals directly are appealing. While protop
 lanetary discs are young and massive they can go through a phase in which 
 their own self-gravity is important driving spiral waves that heat the dis
 c and balance cooling. The large disc masses and strong self-gravity mean 
 that a only a relatively modest concentration of dust is needed for gravit
 ational collapse\, but the highly dynamic environments makes self-gravitat
 ing discs harsh locations for grain growth. I will present on going work o
 n the dynamics of dust in these discs and discuss the conditions required 
 for planetesimal formation. 
LOCATION:MR11\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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