Events

In this talk I will present a selective overview of MURaM simulations conducted in the past 10+ years that range from high-resolution (2km grid spacing) simulations of solar granulation to active region scale simulations with domain extents beyond 300Mm. While a decade ago there was a significant discrepancy in the quiet Sun field strength inferred form Zeeman and Hanle measurements as well as small-scale dynamo simulations, recent models suggest that a value of <|Bz|> ~60-80G on the tau=1 level gives a realistic representation of the quiet Sun. Such field values are large enough to have dynamical consequences on convection with potential implications for larger scale dynamics on the Sun. Simulations of sunspots have provided a comprehensive picture of sunspot magnetoconvection capturing elements of fine structure including umbral dots, penumbral filaments, light bridges, and the connection to the moat region including moat flows and moving magnetic features. Despite this success the presence and extent of penumbra in sunspot simulations remains critically dependent on boundary conditions. Recent research points to a critical role of the subsurface magnetic field structure. Simulations on the scale of entire active regions have provided testbeds for helioseismic inversions. I provide a few examples constraining flux emergence and flow measurements in the proximity of sunspots. I will conclude with an outlook on ongoing developments, including models of the atmosphere reaching into the corona and GPU computing.

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