Simulating Waves in the Upper Solar Atmosphere with SURYA: A Well-balanced High-order Finite-volume Code

Details Simulating Waves in the Upper Solar Atmosphere with SURYA: A Well-balanced High-order Finite-volume Code Simulating Waves in the Upper Solar Atmosphere with SURYA: A Well-balanced High-order Finite-volume Code

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011apj...732...75f&link_type=abstract

The Astrophysical Journal, Volume 732, Issue 2, article id. 75 (2011).

Astronomy and Astrophysics

Astronomy

Magnetohydrodynamics: Mhd, Methods: Numerical, Sun: Atmosphere, Sun: Chromosphere, Sun: Transition Region, Waves

Scientific paper

We consider the 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 named SURYA. Numerical experiments in both two and three space dimensions involving realistic temperature distributions, driving forces, and magnetic field configurations are described. Diverse phenomena such as mode conversion, wave acceleration at the transition layer, and driving-dependent wave dynamics are observed. We obtain evidence for the presence of coronal Alfvén 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.

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