Institution(s): 1. Denison University
An important question in the study of massive protostars is the physical structure of the star forming region. An extension of the Shu infall model to high masses would suggest the existence of a spherical envelope surrounding a central, massive disk. On the other hand, turbulence, outflows, instabilities, or other forces might disrupt such a disk or prevent one from forming in the first place. Observations of acetylene in ro-vibrational absorption on GEMINI provide spatially constrained observations of high-lying transitions. We model the absorption and compare the model predictions with the observations, in order to constrain the models. The implications for the physical structure are discussed, and future observations to test the results are suggested.