Realistic Magnetohydrodynamical Simulation of Solar Local Supergranulation

TL;DR

This paper presents realistic 3D magnetohydrodynamical simulations of solar surface convection, revealing details about convective structures, thermal stratification, and penetration depths using advanced numerical methods and high-performance computing.

Contribution

It introduces a comprehensive simulation framework for solar magnetoconvection with realistic physics and high spatial resolution, advancing understanding of solar surface dynamics.

Findings

Detailed thermal structure of convective motions

Main scales of convective cells identified

Penetration depths of convection characterized

Abstract

Three-dimensional numerical simulations of solar surface magnetoconvection using realistic model physics are conducted. The thermal structure of convective motions into the upper radiative layers of the photosphere, the main scales of convective cells and the penetration depths of convection are investigated. We take part of the solar photosphere with size of 60x60 Mm in horizontal direction and by depth 20 Mm from level of the visible solar surface. We use a realistic initial model of the Sun and apply equation of state and opacities of stellar matter. The equations of fully compressible radiation magnetohydrodynamics with dynamical viscosity and gravity are solved. We apply: 1) conservative TVD difference scheme for the magnetohydrodynamics, 2) the diffusion approximation for the radiative transfer, 3) dynamical viscosity from subgrid scale modeling. In simulation we take uniform two-dimesional grid in gorizontal plane and nonuniform grid in vertical direction with number of cells 600x600x204. We use 512 processors with distributed memory multiprocessors on supercomputer MVS-100k in the Joint Computational Centre of the Russian Academy of Sciences.