I use and develop numerical models to study plasma physics in the solar atmosphere, the interplanetary space, and stars. The main code I work with is the BATS-R-US generic magnetohydrodynamic (MHD) code, which has been developed at the Center for Space Environment Modeling at the University of Michigan. This code has been developed for over a decade to study plasma physics in the solar system, and I extended its usage to astrophysical problems, such as stellar atmospheres, stellar winds, and exoplanets.
The models I use are computationally expensive and are run using high-performance computing technology on supercomputers, such as the NASA PLEIADES cluster at NASA AMES center (left figure below). The BATS-R-US code also has Adaptive Mesh Refinement (AMR) technology that enables to use dynamic, non-uniform grid in the simulations (right figure below).
