Compared to low-mass star formation, very little is known about<br />
the formation process of high-mass stars that are fundamental<br />
in the evolution of galaxies. It is still much debated <br />
whether high-mass stars form in a manner qualitatively similar to <br />
low-mass stars, and there are two major competing models: <br />
accretion via disks and coalescence of low-mass<br />
(proto)stars. In this talk I will discuss some recent efforts <br />
to differentiate between the two models by observing bipolar <br />
outflows from massive protostars.<br />