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SUMMARY:Review - there and back again: the making and destruction of dusty
  planetesimals - Wurm\, G (Mnster)
DTSTART:20090818T080000Z
DTEND:20090818T084000Z
UID:TALK19469@talks.cam.ac.uk
CONTACT:Mustapha Amrani
DESCRIPTION:A dust particle has to take a number of different roads to be 
 incorporated into a planet. On the constructive side\, collisions gentle e
 nough might stick the particle to other particles and lead to growth of la
 rger objects. Ultimately\, beyond any detail\, this is how planetesimals\,
  km-size precursors to planets and terrestrial planets further on form. \n
 \nCollisions are therefore among the most fundamental processes in planet 
 formation. In detail they have their share in shaping the size distributio
 n and morphology of evolving bodies and to set formation time scales of la
 rger objects in protoplanetary disks. \n\nSticking\, rebound\, fragmentati
 on\, and reaccretion (the latter especially by gas drag) are important res
 ults of individual collisions. How far we can get along the size scale of 
 growth from dust upward and which collisions / conditions would be needed 
 to get to planetesimals will be covered in this talk. \n\nAs the evolving 
 bodies are not isolated in their collisions but embedded in a gaseous prot
 oplanetary disk\, other processes can support\, prevent\, or even undo the
  growth of large bodies. Eventually\, these processes might be of similar 
 importance as the collisional growth and put some dependence of the format
 ion processes to the radial distance from the star within the disk. Planet
 esimal and planet formation does not necessarily proceed the same way all 
 over the disk. I will suggest some thoughts on this. 
LOCATION:Seminar Room 1 Newton Institute
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