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Information - IS12 - GD26/PS2.6 Comparative Terrestrial Planetology: Challenges in Numerical Simulations (co-organized by GD & PS)
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Event Information |
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Over the last decades, numerical models of planetary evolution ranging from global planetary formation and accretion models to the point of detailed calculations of today’s mantle and lithosphere dynamics has been significantly improved. Especially significant progress can be registered in geodynamical modelling, which integrates geophysical observations, geochemical constraints and results from mineral physics into a more and more exhaustive picture how the interior of our Earth works. This interdisciplinary session is addressed to all numerical modellers from the geodynamical community (GD) as well as from the planetary physics community (PS) to motivate themselves to discuss their specific results in the context of all terrestrial planets (and larger satellites). The session aims for comparative numerical studies from fields that study planetary formation (e.g., accretion, differentiation, core formation, early magma ocean), planetary dynamos (e.g., initiation, reversals, cessation) and mantle dynamics (e.g., thermal and chemical convection, onset of convection, convection structure, inner core growth, thermal evolution, rheology, partial melting and volcanic activity, plate tectonics versus stagnant lid convection). What do terrestrial planets (including larger satellites) have in common and how do they differ? Why has the Earth still a running dynamo while Mars and Mercury show remnants of an earlier dynamo activity? Why do Earth, Mars and Moon have dichotomies while the Earth is the only planet with plate tectonics, whereas all others are one-plate planets? The above represents only a small selection of question that may be addressed. Time will be reserved for open discussion and comments to summarize results and to define future efforts in numerical modeling.
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Back to Session Programme
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