2000/10/02 by Scott J. Kenyon, Kenyon, Scott J.
Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0010036
24 pages with 6 figures; to appear in the Proceedings of Galactic Structure, Stars, and the Interstellar Medium, a NASA Legacy meeting, edited by M. D. Bicay and C. E. Woodward
arxiv created 2000/10/02 · arxiv updated 2009/12/01
This paper reviews the theory of protostellar debris disks. After a brief introduction to accretion disk physics, I describe coagulation models of planet formation in the outer regions of planetesimal disks. Coagulation models for the Kuiper Belt produce Pluto-sized objects on timescales of 10-40 Myr. These models yield size distributions which agree with observations of Kuiper Belt objects with red magnitudes, R = 20-27. Velocity stirring models for other debris disk systems demonstrate that 500 km or larger objects can stir the velocities of small objects up to the shattering limit needed to begin a collisional cascade.