Japan Geoscience Union Meeting 2016

Presentation information

Oral

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

[M-GI22] Development of computational sciences on planetary formation, evolution and surface environment

Tue. May 24, 2016 10:45 AM - 12:15 PM A07 (APA HOTEL&RESORT TOKYO BAY MAKUHARI)

Convener:*Junichiro Makino(RIKEN AICS), Yoshi-Yuki Hayashi(Department of Planetology/CPS, Graduate School of Science, Kobe University), Shigeru Ida(Department of Earth and Planetary Science, Graduate School of Science and Technology, Tokyo Institute of Technology), Yuri Aikawa(Center for Computational Sciences, University of Tsukuba), Masaki Ogawa(Division of General Systems Studies, Graduate School of Arts and Sciences, University of Tokyo), Masayuki Umemura(Center for Computational Sciences, University of Tsukuba), Chair:Masaki Ogawa(Division of General Systems Studies, Graduate School of Arts and Sciences, University of Tokyo)

11:00 AM - 11:15 AM

[MGI22-07] Modeling the evolving interiors of planets

*Masaki Ogawa1 (1.Division of General Systems Studies, Graduate School of Arts and Sciences, University of Tokyo)

Keywords:mantle evolution, mantle convection, magmatism

There is a clear correlation between the size of a terrestrial planet and the style of tectonic activities that are caused by mantle convection in that planet: There is no clear indication of tectonic activities on the present Moon where the Rayleigh number of the mantle is below the critical Rayleigh number; plume magmatism has occurred almost throughout its 4.5 Gyr history on Mars where the Rayleigh number marginally exceeds the critical value; plume magmatism and tectonic activities are pervasive on the present Earth and Venus where the Rayleigh number is well above the critical value. To develop a comprehensive model of tectonic activities and evolution of these planets, it is necessary to systematically explore the elementary processes that exert control over mantle dynamics. Through my two-dimensional models of magmatism in convecting mantle, I have listed several crucial elementary processes: (1) the magmatism-mantle upwelling feedback that operates in Mars, Venus, and the Earth; (2) mantle bursts that occurs in the Earth and Venus owing to an interaction between magmatism and a high pressure induced solid-solid phase transition of mantle materials; (3) plate tectonics that occurs on the Earth probably because of the ocean that the planet hosts. Here, I argue that a three-dimensional modeling of these processes is necessary for ultimate understanding of mantle evolution in terrestrial planets.