Terrestrial Planet Formation I. The Transition from Oligarchic Growth to Chaotic Growth

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dc.creatorKenyon, Scott J.
dc.creatorBromley, Benjamin C.
dc.date2005-03-25
dc.date2005-11-17
dc.date.accessioned2026-07-07T11:29:38Z
dc.date.available2026-07-07T11:29:38Z
dc.descriptionWe use a hybrid, multiannulus, n-body-coagulation code to investigate the growth of km-sized planetesimals at 0.4-2 AU around a solar-type star. After a short runaway growth phase, protoplanets with masses of roughly 10^26 g and larger form throughout the grid. When (i) the mass in these `oligarchs' is roughly comparable to the mass in planetesimals and (ii) the surface density in oligarchs exceeds 2-3 g/sq cm at 1 AU, strong dynamical interactions among oligarchs produce a high merger rate which leads to the formation of several terrestrial planets. In disks with lower surface density, milder interactions produce several lower mass planets. In all disks, the planet formation timescale is roughly 10-100 Myr, similar to estimates derived from the cratering record and radiometric data.
dc.descriptionAstronomical Journal, accepted; 22 pages + 15 figures in ps format; eps figures at http://cfa-www.harvard.edu/~kenyon/dl/ revised version clarifies evolution and justifies choice of promotion masses
dc.identifierhttps://arxiv.org/abs/astro-ph/0503568
dc.identifierhttp://arxiv.org/abs/astro-ph/0503568
dc.identifierAstron.J.131:1837-1850,2006
dc.identifierdoi:10.1086/499807
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/196777
dc.subjectAstrophysics
dc.titleTerrestrial Planet Formation I. The Transition from Oligarchic Growth to Chaotic Growth
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