The multifaceted planetesimal formation process

  title={The multifaceted planetesimal formation process},
  author={A. Johansen and J. Blum and Hidekazu Tanaka and C. Ormel and M. Bizzarro and H. Rickman},
  journal={arXiv: Earth and Planetary Astrophysics},
Accumulation of dust and ice particles into planetesimals is an important step in the planet formation process. Planetesimals are the seeds of both terrestrial planets and the solid cores of gas and ice giants forming by core accretion. Left-over planetesimals in the form of asteroids, trans-Neptunian objects and comets provide a unique record of the physical conditions in the solar nebula. Debris from planetesimal collisions around other stars signposts that the planetesimal formation process… Expand
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1981)Progress of Theoretical Physics Supplement
  • 1981
2007)Protostars and Planets V
  • 2007
in:Chondrites and the Protoplanetary Disk
  • vol. 341 of Astronomical Society of the Pacific Con-
  • 2005