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Center for Nonlinear Studies |
I will be presenting recent explorations of the turbulent fragmentation paradigm of star formation, through the use of high resolution Adaptive Mesh MHD simulations of turbulent, self gravitating clouds. Adaptive Mesh simulations are necessary to probe the large range of scales in both density and size necessary for a complete description of star formation. I primarily focus on density and magnetic distributions of the gas, as well as gravitationally bound prestellar cores. Prestellar cores are the dense initial conditions for star formation, and we find excellent agreement in with recent radio observations of prestellar cores in a number of physical quantities. These simulations demonstrate that the turbulent fragmentation model with weak magnetic fields are quite successful in explaining star formation.
Host: Hui Li, T-2, 5-3131