  The formation of massive stars may take place at relatively low accretion
rates over a long period of time if the accretion can continue past the onset
of core hydrogen ignition. The accretion may continue despite the formation of
an ionized HII region around the star if the HII region is small enough that
the gravitational attraction of the star dominates the thermal pressure of the
HII region. The accretion may continue despite radiation pressure acting
against dust grains in the molecular gas if the momentum of the accretion flow
is sufficient to push the dust grains through a narrow zone of high dust
opacity at the ionization boundary and into the HII region where the dust is
sublimated. This model of massive star formation by continuing accretion
predicts a new class of gravitationally-trapped, long-lived hypercompact HII
regions. The observational characteristics of the trapped hypercompact HII
regions can be predicted for comparison with observations.
