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Comets and Planetesimal Formation
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In this chapter, we review the processes involved in the formation of planetesimals and comets. We will start with a description of the physics of dust grain growth and how this is mediated by gas-dust interactions in planet-forming disks. We will then delve into the various models of planetesimal formation, describing how these planetesimals form as well as their resulting structure. In doing so, we focus on and compare two paradigms for planetesimal formation: the gravitational collapse of particle over-densities (which can be produced by a variety of mechanisms) and the growth of particles into planetesimals via collisional and gravitational coagulation. Finally, we compare the predictions from these models with data collected by the Rosetta and New Horizons missions and that obtained via observations of distant Kuiper Belt Objects.
Forward citations
Cited by 3 Pith papers
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Considering contact forces during the formation of planetesimals by gravitational collapse: mutual orbits, spin states, and shapes
Soft-sphere contact simulations of gravitationally collapsing pebble clouds form binary planetesimal systems and resolve, for the first time, their spins and shapes.
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Polydisperse Formation of Planetesimals: The dust size distribution in clumps
Polydisperse streaming instability simulations show dense dust clumps have a peaked size distribution, with the largest grains pushed just outside the densest regions.
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A unique solution to overcome the barriers to planetesimal formation at low dust-to-gas ratio
Fully resolved Keplerian turbulence concentrates pebbles into clumps and reduces their radial drift, potentially bypassing the drift and fragmentation barriers to planetesimal formation at canonical dust-to-gas ratios.
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