The general context of this project is the study of the very early phases of evolution of low mass stars and brown dwarfs, following the dynamical phase of gravitational collapse and fragmentation of a molecular cloud which produces a pre-stellar core and an accretion disk. The physical properties of the newly born protostar/proto-brown dwarf crucially depend on two physical processes: accretion from the disk and internal convection which is the most important energy transport in the protostellar interior.
To describe these processes, our team is developing a multi-dimensional, time implicit, hydrodynamical code. Time implicit simulations are required for the description of characteristic stellar evolution processes which proceed on timescales much longer than the dynamical timescale. The main goal of this project is to participate to the development of the implicit hydrodynamical code and to study the properties of interior convection in accreting objects.