Based on three dimensional AMR simulations we show that the assembly
of prestellar cores which will result in massive stars is a very rapid
process. We find mass typical accretion rates which are high enough to
squeeze the radiation field produced by the young massive star.
Initial turbulence and funnelled accretion through filaments
furthermore enhances accretion onto the central object. We also show
that bipolar outflows will be launched already in a very early stage
of the prestellar evolution if the inital molecular core is threaded
with magnetic fields. These magnetically driven outflows produce cavities
out of which radiation pressure can be released, thereby reducing the
limitations on the final mass of massive stars formed by gravitational
collapse.
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