This program examines fundamental problems of the physics of magnetic field dynamics in the heliosphere. Areas of current interest in solar physics include the emergence of magnetic flux from the convection zone into the corona and the energization of coronal mass ejections. Areas of current interest in magnetospheric physics are focused on magnetopause reconnection and magnetic instabilities. Areas of current interest in solar wind physics include the acceleration of the slow solar wind, the generation of magnetic fluctuations in the solar wind, and the propagation of coronal mass ejections through the solar wind. The research makes extensive use of time-dependent numerical simulations using one-, two-, and three-dimensional numerical models. Much of the work focuses on determining observables for comparison with existing and anticipated satellite data in the visible, ultraviolet, and X-ray regions of the spectrum, as well as with in-situ data. Computing capabilities include access to DOD high-performance computing facilities.