Numerical simulations of astrophysical turbulence

Turbulence is a crucial component of dynamics of astrophysical fluids dynamics, including those of ISM, clusters of galaxies and circumstellar regions. The knowledge of turbulence properties is essential for understanding star formation, molecular chemistry, cosmic ray transport and acceleration, transport of heat and angular momentum etc. I shall show that a substantial progress in understanding major astrophysical processes is possible if we know very basic properties of the magnetized turbulent flow, e.g., its spectrum. I shall show that more subtle properties can be obtained if we also know turbulent intermittency. I shall discuss theoretical models, their numerical testing and the practically important astrophysical implications of the magnetized turbulence. (author)