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A 1D-spherical cloud collapse to form a massive star is eventually stopped by the radiation pressure of the new born star. A disk structure with cavities and a massive accretion disk is essential to transport sufficient material onto the star beyond the 1D radiation pressure limit.
Yet, even the 2D simulations indicate a low efficiency, e.g. very massive disks (120Msol) are needed to form a 43Msol star.
In our project we determine the effects of dimensionality (3D vs. 2D), combined with physical effects, e.g. radiation pressure, magnetic fields and self-gravity on the accretion rate as a function of disk mass and primary mass/luminosity. For that purpose we have developed a 2/3D- (magneto-) hydrodynamical code, including self-gravity, Flux-Limited Diffusion of radiation combined with ray-tracing irradiation.
Here we present our first simulation results and the current state of the project.
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