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We present radiation hydrodynamics simulations of the collapse of massivepre-stellar cores. We treat frequency dependent radiative feedback from stellarevolution and accretion luminosity at a numerical resolution down to 1.27 AU.In the 2D approximation of axially symmetric simulations, it is possible forthe first time to simulate the whole accretion phase (up to the end of theaccretion disk epoch) for the forming massive star and to perform a broad scanof the parameter space. Our simulation series show evidently the necessity toincorporate the dust sublimation front to preserve the high shielding propertyof massive accretion disks. While confirming the upper mass limit ofspherically symmetric accretion, our disk accretion models show a persistenthigh anisotropy of the corresponding thermal radiation field. This yields tothe growth of the highest-mass stars ever formed in multi-dimensional radiationhydrodynamics simulations, far beyond the upper mass limit of sphericalaccretion. Non-axially symmetric effects are not necessary to sustainaccretion. The radiation pressure launches a stable bipolar outflow, whichgrows in angle with time as presumed from observations. For an initial mass ofthe pre-stellar host core of 60, 120, 240, and 480 Msun the masses of the finalstars formed in our simulations add up to 28.2, 56.5, 92.6, and at least 137.2Msun respectively.

Circumventing the radiation pressure barrier in the formation of massive stars via disk accretion