Nagoya University, Japan
Recent observations have emphasized the importance of the formation and evolution of magnetized filamentary molecular clouds in the process of star formation. Theoretical and observational investigations have provided convincing evidence for the formation of molecular cloud cores by the gravitational fragmentation of filamentary molecular clouds. The size and total angular momentum of a protoplanetary disk are supposed to be related directly to the rotational property of the parental molecular cloud core where the central protostar and surrounding disk are born. In this review we summarize our current understanding of various processes that are required in describing the filamentary molecular clouds and try to understand the origin of angular momenta of molecular cloud cores and its link to the mass function of cores and the stellar initial mass function.
2019 September 18, 13:30
Centro de Astrofísica da Universidade do Porto (Auditorium)
Rua das Estrelas, 4150-762 Porto