Advanced Astrophysical Fluid Dynamics The goal of the course is to understand: (a) fluid dynamics and magnetohydrodynamics (MHD), (b) waves and instabilities, (c) global and local helioseismology, (c) shocks, solar wind, accretion, (d) fundamental aspects of turbulence and convection, (e) dynamo theory, and (f) numerical techniques for MHD and turbulence. Course description: Solar/terrestrial connection, radial structure, equations, Atmospheric waves (p and g modes), numerical techniques, Helioseismology, Abel's integral equation Supersonic flows, energy conservation, Magnetic fields, magnetic support and coronal mass ejections, Thin accretion disc physics: steady, time-dependent Alfven waves, slow, fast, and MRI Laminar and turbulent dynamos, Dimensional analysis, blast waves, Convection, mixing length, turbulence, Magnetic reconnection, Computer exercises: waves and energy conservation, dynamo and magnetic helicity, Alfven waves, Parker wind, magnetic relaxation, mean-field dynamo models Teachers: Axel Brandenburg, and people from his group Literature: S.N. Shore: Astrophysical Hydrodynamics A.R. Choudhuri: The Physics of Fluids and Plasmas Examination: The assessment will be based on weekly exercises, and a final report summarizing the results from computer exercises. Prerequisite: Maxwell equations, basic fluid dynamics, some familiarity with programming would be useful Preliminary schedule: see http://www.nordita.org/~brandenb/teach/MHD/schedule/2013_Feb.html