Professor Hartmann studies the processes by which cold clouds of gas and dust fragment and then collapse, forming stars and a surrounding rotating disk; and the evolution of disks which ultimately can form planets. Because protostellar clouds form in complex, highly structured and turbulent gas, time-dependent (magneto)hydrodynamics is required to follow fragmentation and collapse to stars and disks. Similarly, the evolution of planet-forming disks involves both gravitational and magnetic turbulence. Simulations of cloud and disk evolution over the necessary timescales (105 to 106 years) with reasonable resolution demands extensive parallel processing.
Research AreasHigh Performance Computing