From filaments to outflows in magnetized molecular clouds

Ralph Pudritz (McMaster University) - Feb 4, 2008 at 12:10 pm

Turbulent fragmentation of gas in molecular clouds by supersonic turbulence has the potential to provide a comprehensive theory of star formation. A heirarchy of physical processes involved: from the formation of large scale filaments in shocks, to the growth of star-forming cores within them. On smaller scales, the collapse of overdense asymmetric cores into disks and the early appearance of outflows become important for understanding binary formation and star formation efficiencies. Magnetic fields can play an important role on all of these physical scales - from controlling the degree of fragmentation to enabling the appearance of outflows. I present the results of our recent 3D numerical simulations of magnetized, cooling, self-gravitating, cluster forming regions in molecular clouds. We make contact with results of recent observations of the mass functions and magnetic fields of cores, as well as the appearance of outflows in the earliest stages of gravitational collapse and disk formation.

The seminar will be held in 544 Campbell Hall.


Return to seminar schedule