Kavli Affiliate: Robert Cameron
| First 5 Authors: Veronika Witzke, Alexander I. Shapiro, Nadiia M. Kostogryz, Lucien Mauviard, Tanayveer S. Bhatia
| Summary:
Three-dimensional (3D) radiative magnetohydrodynamics (MHD) simulations are
the only way to model stellar atmospheres without any ad hoc parameterisations.
Several 3D radiative MHD codes have achieved good quantitative agreement with
observables for our Sun. We aim to validate the most up-to-date version of the
MURaM code against well established quiet Sun measurements, in particular
spatially averaged measurements that are relevant for stellar studies. This
validation extends the number of solar observables that MURaM can reproduce
with high precision. It is also an essential condition for using MURaM to
accurately calculate spectra of other cool stars. We simulate the solar upper
convection zone and photosphere harbouring a small-scale-dynamo. Using time
series of 3D snapshots we calculate the spectral irradiance, limb darkening and
selected spectral lines, which we compare to observations. The computed
observables agree well with the observations, in particular the limb darkening
of the quiet Sun is reproduced remarkably well.
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