Haruhisa Iijima (Nagoya University) Kanya Kusano (Nagoya University)
The solar convection zone is significantly stratified. The density at the base of the convection zone is 1 million times larger than that at the surface. This strong stratification causes significant scale separation between the deep convection zone and the near surface layer. The length scale at the base is 200 Mm and 1 Mm at the surface. The time scales in these layers are one month and minutes respectively. Covering these broad scale-ranges in numerical simulation is difficult. The global magnetic field is thought to be generated in the deep convection zone, and the resulting sunspot appears at the surface. Except for the helioseismology, the observation only detects the phenomena above the photosphere. The connection between the deep convection zone and the surface is in demand. In this study, we develop a new code R2D2 (Radiation and RSST for Deep Dynamics), for covering the whole convection zone and for the first time succeed in doing it. The R2D2 treat realistic radiation transfer around the photosphere as well as adequate treatment of the deep convection zone. In the presentation, we show our latest result of the whole convection zone simulation. Influence of the photosphere on the deep convection structure and the flux emergence from the deep convection zone to the surface are shown.
Mode of presentation: oral (Need to be confirmed by the SOC)