N-Body Simulations of Late Stage Planetary Formation with a Simple Fragmentation Model |
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| Institution: | 1. Key Lab of Submarine Geosciences and Prospecting Techniques, MOE, Institute for Advanced Ocean Study, College of Marine Geosciences, Ocean University of China, Qingdao 266100, China;2. Laboratory for Marine Geology, Qingdao National Laboratory for Marine Science and Technology, Qngdao 266061, China;3. Institute of Geology, Chinese Academy of Geological Sciences, Beijing 100037, China;4. UCD School of Earth Sciences, University College Dublin, Belfield, Dublin 4, Ireland;1. Université de Lyon, Laboratoire Magmas et Volcans, UJM-UBP-CNRS-IRD, 23 rue Dr. Paul Michelon, 42023 Saint Etienne, France;2. J.W. Goethe Universität, Institut für Geowissenschaften, Altenhöferallee 1, D-60438 Frankfurt am Main, Germany;3. Université de Liège, Département de Géologie B20, Quartier Agora, allée du six Août 12, B-4000 Liège, Belgium;4. Université de Genève, Département des Sciences de la Terre, rue des Maraichers, 13, 1205 Genève, Switzerland;5. GET, UMR 5563 CNRS/UR 234 IRD/UPS, 14, avenue Édouard Belin, 31400 Toulouse, France;6. Univ d''Orléans, ISTO, UMR 7327, 45071 Orléans, France;7. Université de Lyon, Université Lyon 1, ENS de Lyon, CNRS, UMR 5276 LGL-TPE, F-69622 Villeurbanne, France;1. State Key Lab for Geological Processes and Mineral Resources, China University of Geosciences, Wuhan 430074, China;2. Center for Global Tectonics, School of Earth Sciences, China University of Geosciences, Wuhan 430074, China;3. Department of Earth and Environmental Sciences, University of Windsor, Ontario, Canada;4. Department of Geology, University of Leicester, U.K;5. Department of Geosciences, University of Houston, TX, USA;6. University of California Davis, University College, Oxford, United Kingdom;7. Department of Atmospheric and Environmental Sciences, University at Albany, USA;8. Earth-Life Institute, Tokyo Institute of Technology, Japan |
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| Abstract: | We present results of two-dimensional gravitationalN-body simulations of the late stage of planetary formation. This stage is characterized by the direct accretion of hundreds of lunar-sized planetesimals into planetary bodies. Our simulation code is based on the Hermite Individual Timestep integration algorithm, and gravitational interactions among all bodies are included throughout the simulations. We compare our simulation with earlier works that do not include all interactions, and we find very good agreement. A previously published collisional fragmentation model is included in our simulation to study the effects of the production of fragments on the subsequent evolution of the larger planetary bodies. It is found that for realistic two-body collisions that, according to this model, both bodies will suffer fragmentation, and that the outcome of the collision will be a relatively large core containing most of the mass and a few small fragments. We present the results of simulations that include this simple fragmentation model. They indicate that the presence of small fragments have only a small effect on the growth or orbital evolution of the large planet-sized bodies. |
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