Japan Geoscience Union Meeting 2019

Presentation information

[J] Poster

M (Multidisciplinary and Interdisciplinary) » M-GI General Geosciences, Information Geosciences & Simulations

[M-GI35] Development of computational sciences on planetary formation, evolution and surface environment

Tue. May 28, 2019 3:30 PM - 5:00 PM Poster Hall (International Exhibition Hall8, Makuhari Messe)

convener:Yoshi-Yuki Hayashi(Department of Planetology/CPS, Graduate School of Science, Kobe University), Masaki Ogawa(Division of General Systems Studies, Graduate School of Arts and Sciences, University of Tokyo), Shigeru Ida(Earth-Life Science Institute, Tokyo Institute of Technology), Kanya Kusano(Institute for Space-Earth Environmental Research, Nagoya University)

[MGI35-P02] Attempts at numerical modeling of 3-D mantle convection with magmatism and plate tectonics

*Masanori Kameyama1,2, Masaki Ogawa3,2, Takehiro Miyagoshi2, Takatoshi Yanagisawa2 (1.Geodynamics Research Center, Ehime University, 2.Japan Agency for Marine-Earth Science and Technology, 3.University of Tokyo at Komaba)

Keywords:rocky planets, mantle dynamics, mantle magmatism, plate tectonics

We are developing 3-D numerical models of mantle convection including the effects of mantle magmatism and plate tectonics, in order to deepen the insights into the thermo-chemical evolution of the mantles of terrestrial bodies. The mantle magmatism is modeled by the generation of liquid phase (magma) owing to the pressure-release melting induced by ascending flows of solid-state convection and the motion of the generated magma as a permeable flow through the solid matrix driven by a buoyancy due to the density difference between the solid and the liquid phases. The coherent motion of tectonic plates is, on the other hand, helped by the narrow zones of low viscosity within the highly viscous "lithosphere" along the top cold surface generated by the stress-history-dependent rheology. However, despite their crucial roles in controlling the overall flow structures, these two mechanisms are incompatible with the solid-state convection of the mantle in essence from the numerical aspects: the localized irregularities caused by them severely deteriorate the large-scale numerical solution of solid-state convection particularly by the multigrid method. In this presentation, we will show the current status and outcrops of our attempts to overcome the numerical difficulty, together with some examples of 3-D experiments running on massive (super)computers.