Japan Geoscience Union Meeting 2019

Presentation information

[E] Poster

A (Atmospheric and Hydrospheric Sciences ) » A-OS Ocean Sciences & Ocean Environment

[A-OS11] Continental-Oceanic Mutual Interaction: Planetary scale Material Circulation

Wed. May 29, 2019 5:15 PM - 6:30 PM Poster Hall (International Exhibition Hall8, Makuhari Messe)

convener:Yosuke Alexandre Yamashiki(Earth & Planetary Water Resources Assessment Laboratory Graduate School of Advanced Integrated Studies in Human Survivability Kyoto University), Yukio Masumoto(Graduate School of Science, The University of Tokyo), Swadhin Behera(Climate Variation Predictability and Applicability Research Group, Application Laboratory, JAMSTEC, 3173-25 Showa-machi, Yokohama 236-0001), Takanori Sasaki(Department of Astronomy, Kyoto University)

[AOS11-P04] Numerical simulation of Tidal Heating using SPH and its application to inner sea formation

*keiya murashima1, Yosuke Alexandre Yamashiki1, Natsuki Hosono2 (1.Kyoto University, 2.Japan Agency for Marine-Earth Science and Technology)

Keywords:icy moon, tidal heating

There are some traces of liquid in icy moons, such as a plume of vapor of Europa acquired by Hubble Space Telescope and tiger stripes of Enceladus observed by Cassini. Since liquid water is essential for the origin of life, it can be important to understand the development of inner sea and also the temperature distribution inside of such icy moons.

It is considered that the tidal heating caused by tidal acceleration melts the inner icy layer which results in the presence of liquid water beneath its surface. Thus, we aim at simulating the tidal heating of an icy moon by 3-dimensional numerical fluid calculation in Smoothed Particle Hydrodynamics (SPH) method. As the tidal heating model, we apply the viscosity model which was used for numerical calculation of tidal stripping.

It is confirmed that this viscosity model lead to qualitatively correct result about tidal disruption, but the possibility of its application to tidal heating is not validiated. Therefore, as a first step, we tried to compare the result of this simulation with the result which is estimated theoretically. We made a rotation of a differentiated Titan-sized tidally locked object around a Saturn-mass material point with the radius of orbit being 1.1 times larger than its Roche limit. We also considered how to applicate this simulation to the calculation of actual icy moons. We will report the progress.