To calculate the formation of an entire planetary system, a computer
code must combine the best of the coagulation
and n-body algorithms. Our multiannulus hybrid
code includes coagulation for the small objects and n-body integrations
for the largest objects. Our hybrid code links to two methods together
and can follow the evolution of objects ranging in size from 1 micron
up to 10,000 km.
We are applying the code to understand planet formation in a variety
of circumstances. The links describe some of our ongoing projects.
Icy exoplanets and debris disks
Kuiper belt objects
Simulations for the GMT