Abstract


  USING GRAPHICAL PROCESSING UNITS TO SIMULATE THE DYNAMICS GENERATED BY SOLAR GLOBAL OSCILLATING EIGENMODES GENERATED IN THE SOLAR ATMOSPHERE

  M. Griffiths, The University of Sheffield, m.griffiths@sheffield.ac.uk
  V. Fedun, The University of Sheffield, v.fedun@sheffield.ac.uk
  R. Erdelyi, The University of Sheffield, robertus@sheffield.ac.uk

The solar atmosphere exhibits a diverse range of wave phenomena. One of the earliest discovered was the five-minute oscillations attributed to pressure-driven acoustic modes. These acoustic (p) modes are generated by just beneath the photosphere. The resulting propagation and leakage of this wave energy into the solar atmosphere may be used as a diagnostic tool to predict some of the physical characteristics of the solar atmosphere.

In this talk we will report on the current development of SMAUG (Sheffield MHD Accelerated Using GPUs) code and show the results of a series of hydrodynamical simulations of wave
excitation and propagation in the quiet solar atmosphere. First, we describe the MHD code SMAUG (Sheffield MHD Accelerated Using GPUs) developed to run the ensemble of simulations and present a recent progress enabling the MHD code to utilise multiple GPUs. Next, we address the remote visualisation techniques employed for the analysis of the results.

With the objective of recreating atmospheric motions generated by global resonant oscillation, the we used a spatially structured driver across the base of the computational model. The main idea of performed modeling is to understand how the energy supplied by various wave modes is redistributed in the atmosphere. We shed light on the mechanisms leading to ubiquitous intensity oscillations in the stratified solar atmosphere and establish a link between signals at photospheric levels and the solar corona response.