Abstract
There has been tremendous progress in the degree of realism of three-dimensional radiation magneto-hydrodynamic simulations of the solar atmosphere in the past decades. Four of the most frequently used numerical codes are Bifrost, CO5BOLD, MANCHA3D and MURaM. Here we test and compare the wave propagation characteristics in model runs from these four codes by measuring the dispersion relation of acoustic-gravity waves at various heights. We find considerable differences between the various models. The height dependence of wave power, in particular of high-frequency waves, varies by up to two orders of magnitude between the models, and the phase difference spectra of several models show unexpected features, including ±180° phase jumps. This article is part of the Theo Murphy meeting issue 'High-resolution wave dynamics in the lower solar atmosphere'.
Highlights
Driven by the tremendous increases in computational resources over the past decades, computational astrophysics has become an important and rapidly growing discipline of astronomy, including solar physics
In an effort to benchmark the dynamics in simulations of the solar atmosphere, we have compared the wave propagation characteristics in various model runs produced with the Bifrost, CO5BOLD, MANCHA3D and MURaM codes
We have studied the height dependence of wave power in the various models, compared 1-D phase difference spectra between selected heights, and investigated the phase propagation of acoustic gravity waves from layer to layer, bottom to top, of the simulations
Summary
Driven by the tremendous increases in computational resources over the past decades, computational astrophysics has become an important and rapidly growing discipline of astronomy, including solar physics. Four of the most frequently used numerical codes are Bifrost [14, 15], CO5BOLD [16], MANCHA3D [17, 18, 19], and MURaM [20, 21] Some of these models were benchmarked for their average properties in the near-surface layers, by comparing their average stratifications as well as their temporal and spatial fluctuations (e.g., the root mean square (RMS) of granular contrast and vertical velocities) [22].
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