TY - JOUR
T1 - High-Accuracy Statistical Simulation of Planetary Accretion
T2 - II. Comparison with N-Body Simulation
AU - Inaba, Satoshi
AU - Tanaka, Hidekazu
AU - Nakazawa, Kiyoshi
AU - Wetherill, George W.
AU - Kokubo, Eiichiro
N1 - Funding Information:
We express our gratitude to S. Ida for helpful discussion. We also thank H. Emori and S. J. Kortenkamp for continuous encouragement. This work has been supported by a Grant-in-Aid for General Scientific Research (B) (No. 09440089) and by NASA Grants NAG5-6873, NAG5-4285, and NAG5-6977. S. Inaba is grateful for financial support from the Japan Society for Promotion of Science (JSPS Postdoctoral Fellowships for Research Abroad, 1999– 2001). The computation has been performed on Cray C916 at the Computer Center of Tokyo Institute of Technology and a Alpha PC at the Carnegie Institution of Washington.
PY - 2001/1
Y1 - 2001/1
N2 - We have constructed an improved statistical method for the calculation of planetary accumulation using the currently standard model of terrestrial planet formation and using the latest results of planetary dynamical theory. The method is applicable for the range of masses in which velocity changes are dominated by gravitational forces, mutual collisions, and gas drag. Calculations are reported both with and without nebular gas. This method has been compared with N-body simulations, and the results of the two calculations are in agreement. As in earlier calculations, the growth of bodies in this mass range and at 1 AU occurs on a ~105 year time scale and is characterized by the evolution of an initially continuous mass distribution into a bimodal distribution, the high mass end of which consists of runaway bodies in the size range of ~1026 g. In this general way, these results are in agreement with those reported earlier (e.g., Wetherill and Stewart 1993, Icarus106, 190-209), but significant differences are also found as a result of the greater precision of the collision rate and the velocity evolution rate of planetesimals used in the present work.
AB - We have constructed an improved statistical method for the calculation of planetary accumulation using the currently standard model of terrestrial planet formation and using the latest results of planetary dynamical theory. The method is applicable for the range of masses in which velocity changes are dominated by gravitational forces, mutual collisions, and gas drag. Calculations are reported both with and without nebular gas. This method has been compared with N-body simulations, and the results of the two calculations are in agreement. As in earlier calculations, the growth of bodies in this mass range and at 1 AU occurs on a ~105 year time scale and is characterized by the evolution of an initially continuous mass distribution into a bimodal distribution, the high mass end of which consists of runaway bodies in the size range of ~1026 g. In this general way, these results are in agreement with those reported earlier (e.g., Wetherill and Stewart 1993, Icarus106, 190-209), but significant differences are also found as a result of the greater precision of the collision rate and the velocity evolution rate of planetesimals used in the present work.
KW - Computer techniques
KW - N-body simulation.
KW - Planetary accretion
KW - Planetary formation
KW - Planetesimals
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U2 - 10.1006/icar.2000.6533
DO - 10.1006/icar.2000.6533
M3 - Article
AN - SCOPUS:0000391072
SN - 0019-1035
VL - 149
SP - 235
EP - 250
JO - Icarus
JF - Icarus
IS - 1
ER -