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Proposing Institution

ITA Heidelberg
Project Manager

Prof. Dr. Ralf S. Klessen
Albert-Ueberle-Str. 2
69120 Heidelberg
Supersonic random motions in star-forming molecular clouds create the seeds for gravitational collapse into proto-stellar cores and subsequently into stars. Self-gravity must be the physical mechanism for the final transition of dense gas into bound, proto-stellar cores and stars. Magnetic fields, ubiquitously observed in nearby molecular clouds, may also play an important role in this process. To advance on these issues, we use self-consistent, 3-dimensional hydrodynamical and magnetohydrodynamical simulations of solenoidally (divergence-free) and compressively (curl-free) driven supersonic turbulence, including self-gravity and magnetic fields to investigate the formation of dense clumps and bound cores in an environment typical for interstellar gas clouds. A long-standing problem in astrophysics is explaining the observed distribution of core masses (Core Mass Function, CMF) and stellar masses (stellar Initial Mass Function, IMF). Continuing our studies of purely non-gravitational turbulent fragmentation, we investigate the mechanisms of turbulent gravitational fragmentation, termed gravo-turbulent fragmentation. We will furthermore include magnetic fields in these simulations to check the validity of analytic theories explaining the CMF and IMF. The final goal of our simulations is the correct prediction of the distribution of cores and stellar masses, and evaluating the role of magnetic fields for these distributions.

Impressum, Conny Wendler