Computation has become an essential tool in theoretical astrophysics, data analysis, and modeling, and Princeton is a world leader in the development and application of numerical methods in astrophysics. Researchers at Princeton use scientific computation to study an enormous range of physical processes. At the largest scales, N-body, hydrodynamic, and radiative transfer methods are used to study cosmological structure formation, galaxy formation, and reionization (Cen, J. Ostriker). This work has helped establish the modern theory of the Lyman alpha forest (Cen, J. Ostriker). At the smallest scales, particle-in-cell (PIC) methods are used to follow particle acceleration, kinetic turbulence, and microscale instabilities in dilute astrophysical plasmas ('Spitkovsky, Kunz). In between, a wide variety of numerical methods are used to understand core-collapse supernova explosions (Burrows), accretion onto compact objects (Burrows, 'Spitkovsky, 'Stone), gravitational fragmentation of molecular clouds and star formation ('Stone, E. Ostriker), accretion disks ('Stone, Kunz), turbulent driving and dissipation in the interstellar medium (E. Ostriker) and the solar wind (Kunz), and the light scattering properties of interstellar dust grains (Draine), just to name a few.