Stellar Mass Accretion Rates from Fragmentation of a Rotating Core

摘要: We investigate the details of protostellar mass accretion, \(\dot{M}\), during collapse isolated, initially uniformly rotating, low-mass cores, using hydrodynamic models star formation. The assumption rigid rotation is supported by recent observations that there no apparent correlation between level turbulence and fragmentation in dense suggesting works mainly before gravitationally bound pre-stellar cores form their inner parts are likely to be velocity coherent. perform high-resolution calculations Smoothed Particle Hydrodynamics (SPH) code GADGET-2, modified inclusion sink particles. compare our results with theoretical formation based on gravoturbulent observational data. find small scales low-mass, accretion statistical properties resulting stellar ensembles bear little dependence whether contracting gas turbulent or rotating as a whole.