  I compare theoretical models of massive star formation with observations of
the Orion Hot Core, which harbors one of the closest massive protostars.
Although this region is complicated, many of its features (size, luminosity,
accretion disk, HII region, outflow) may be understood by starting with a
simple model in which the star forms from a massive gas core that is a coherent
entity in approximate pressure balance with its surroundings. The dominant
contribution to the pressure is from turbulent motions and magnetic fields. The
collapse can be perturbed by interactions with other stars in the forming
cluster, which may induce sporadic enhancements of the accretion and outflow
rate.
