Abstract

It is well-established that bound multiple-star systems are the norm at all stellar evolutionary stages, and the frequency of multiple-star systems appears to increase toward younger stellar ages. These protostellar binary and higher-order systems are the result of collapse and fragmentation of their natal clouds and cores. Disks around some stars fragment and create protostellar companions, while other multiples form through dynamical evolution. Understanding these processes requires an understanding of the interplay between several highly non-linear physical processes, including gravity, turbulent hydrodynamics, and electromagnetism. This necessitates the use of numerical simulations in order to model multiplicity in star-forming regions. This talk discusses the methods and results of three recently completed large-scale simulations of magnetized clouds, which are part of a larger ongoing effort to understand how different global properties of clouds affect the properties of the resulting multiple-star systems.