Ice Lines , Planetesimal Composition and Solid Surface Density in the Solar Nebula

  title={Ice Lines , Planetesimal Composition and Solid Surface Density in the Solar Nebula},
  author={Sarah E. Dodson-Robinson},
  • Sarah E. Dodson-Robinson
  • Published 2008
To date, there is no core accretion simulation that can successfully account for the formation of Uranus or Neptune within the observed 2-3 Myr lifetimes of protoplanetary disks. Since solid accretion rate is directly proportional to the available planetesimal surface density, one way to speed up planet formation is to take a full accounting of all the planetesimal-forming solids present in the solar ar X iv :0 80 6. 37 88 v2 [ as tr oph ] 4 D ec 2 00 8 

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