The most massive stars in the galaxy - those with more than 15 to
20 solar masses - are lilkely to ionize their surroundings before
they reach their final mass. How can they accrete in spite of the
presence of over-pressurized gas?
This thesis presents results of Submillimeter Array (SMA) and Very
Large Array (VLA) studies of massive star formation regions in the
early stages of ionization, as well as an analysis of numerical
simulations of the evolution of these young HII regions. The
results favor a picture in which very massive stars form in
accretion flows that are partially ionized and that keep accreting
material from their environment.
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