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SUMMARY:Planetesimal formation: numerical modeling of particle growth\, se
 ttling\, and collective gas-grain interactions - Weidenschilling\, S (Plan
 etary Science Institute)
DTSTART:20090929T080000Z
DTEND:20090929T090000Z
UID:TALK20338@talks.cam.ac.uk
CONTACT:Mustapha Amrani
DESCRIPTION:In a relatively quiescent solar nebula\, solid particles settl
 e to form a dense layer in the midplane. The density of this layer is set 
 by a balance between settling and diffusion caused by shear-generated turb
 ulence. I present results of a numerical model for the equilibrium structu
 re of a layer of particles of arbitrary size or a mixture of sizes. Radial
  drift rates and relative velocities are computed. Another model includes 
 coagulation of particles throughout the thickness of the nebula\; it is us
 ed to determine timescales for growth of aggregates and their settling\, a
 nd the range of impact strength necessary for the production of macroscopi
 c bodies by collisional sticking. Finally\, a model for gravitational coag
 ulation of bodies in Keplerian orbits is used to infer consequences of ini
 tial planetesimal sizes for accretion of planetary embryos. 
LOCATION:Seminar Room 1\, Newton Institute
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