Planetesimal Capture in the Disk Instability Model

Ravit Helled; Morris Podolak; Attay Kovetz

doi:10.1016/j.icarus.2006.06.011

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arXiv · astro-ph/0606726

Planetesimal Capture in the Disk Instability Model

Ravit Helled·Morris Podolak·Attay Kovetz

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Abstract

We follow the contraction and evolution of a typical Jupiter-mass clump created by the disk instability mechanism, and compute the rate of planetesimal capture during this evolution. We show that such a clump has a slow contraction phase lasting ~3x10^5 years. By following the trajectories of planetesimals as they pass through the envelope of the protoplanet, we compute the cross-section for planetesimal capture at all stages of the protoplanet's evolution. We show that the protoplanet can capture a large fraction of the solid material in its feeding zone, which will lead to an enrichment of the protoplanet in heavy elements. The exact amount of this enrichment depends upon, but is not very sensitive to the size and random speed of the planetesimals.

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Ravit Helled, Morris Podolak, Attay Kovetz. 2006-06-29. Planetesimal Capture in the Disk Instability Model. https://doi.org/10.1016/j.icarus.2006.06.011

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