Realistic Modeling of Multi-Scale MHD Dynamics of the Solar Atmosphere

Thursday, 18 December 2014
Irina Kitiashvili1, Nagi Nicolas Mansour1, Alan A Wray1, Seokkwan Yoon1 and Alexander G Kosovichev2, (1)NASA Ames Research Center, Moffett Field, CA, United States, (2)New Jersey Institute of Technology, Edison, NJ, United States
Realistic 3D radiative MHD simulations open new perspectives for understanding the turbulent dynamics of the solar surface, its coupling to the atmosphere, and the physical mechanisms of generation and transport of non-thermal energy. Traditionally, plasma eruptions and wave phenomena in the solar atmosphere are modeled by prescribing artificial driving mechanisms using magnetic or gas pressure forces that might arise from magnetic field emergence or reconnection instabilities. In contrast, our 'ab initio' simulations provide a realistic description of solar dynamics naturally driven by solar energy flow. By simulating the upper convection zone and the solar atmosphere, we can investigate in detail the physical processes of turbulent magnetoconvection, generation and amplification of magnetic fields, excitation of MHD waves, and plasma eruptions. We present recent simulation results of the multi-scale dynamics of quiet-Sun regions, and energetic effects in the atmosphere and compare with observations. For the comparisons we calculate synthetic spectro-polarimetric data to model observational data of SDO, Hinode, and New Solar Telescope.