B. Paxton, L. Bildsten, K. Moore, P. Macias
KITP and Department of Physics
UC-Santa Barbara
MESA
employs modern numerical approaches and is written with
present and future shared-memory, multi-core, multi-thread and possibly
hybrid architectures in mind so that performance always grows. MESA star
combines the numerical and physics modules for simulations of a wide
range of stellar evolution scenarios ranging from very-low mass to
massive stars, including advanced evolutionary phases leading up to
explosions. It simultaneously solves the fully coupled structure and
composition equations. It uses adaptive mesh refinement and
sophisticated timestep controls, and supports shared memory parallelism
based on OpenMP. State-of-the-art modules provide equation of state,
opacity, nuclear reaction rates, and element diffusion, as well as
atmosphere boundary conditions. In this poster, we will show MESA's
recent application to asteroseismology, focusing on modeling the
solar-like oscillator HD49385, a G0 subgiant that was extensively
observed by COROT (Deheuvels et al. 2010) and previously modeled by
Deheuvels and Michel (2011).