Simulating Waves in the Upper Solar Atmosphere with Surya: A Well-Balanced High-Order Finite Volume Code
MARYLAND UNIV COLLEGE PARK CENTER FOR SCIENTIFIC COMPUTATION AND MATHEMATICAL MODELING(CSCAMM)
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We consider propagation of waves in a stratified non-isothermal magnetic atmosphere. The situation of interest corresponds to waves in the outer solar chromosphere and corona and other stellar atmospheres. The waves are simulated by using a high-resolution well-balanced finite volume based massively parallel code termed SURYA. Numerical experiments in both two and three space dimensions involving realistic temperature distributions driving forces and magnetic field configurations are described. Diverse phenomena like mode conversion, wave acceleration at the transition layer and driving dependent wave dynamics are observed. We obtain evidence for the presence of coronal Alfven waves in some three dimensional configurations. Although some of the incident wave energy is transmitted into the corona, a large proportion of it is accumulated in the chromosphere providing a possible mechanism for chromospheric heating.