Astrophysics is an observational science. One must make use of the information given to you: light, neutrinos, and gravitational radiation, to build up a theoretical picture of a system. Simulations allow one to build a model of a system and test different theories, to provide a detailed understanding of a system that compliments the observations. In this class, we will discuss the use of simulations in modern astrophysics. The equations of hydrodynamics will be discussed, as well as the different types of hydrodynamical instabilities that dominate astrophysical flow. This will be followed by a description of popular computational methods for their solution. The basics of numerical methods (interpolation, differentiation, solving ODEs) will be reviewed. Students will practice these ideas on the linear advection equation and the equations of gasdynamics. Classic and modern papers describing the application of computational hydrodynamics will be discussed. Students will also learn how to use popular, publically available hydrodynamics codes, including the FLASH Code.

Knowledge of a programming language is required. Examples will be provided in Fortran, C, and/or python.