Massive Star Formation: Theory Meets Observation

How do massive stars form is still debated. In order to test theories of massive star formation, we present a radiation transfer model consistently developed for a core in high pressure environment forming a massive star through Core Accretion. This model includes collapsing and rotating cores, accretion disks, a disk wind filling the outflow cavity, and protostellar evolution. We compare the SED and multi-wavelength outflow-axis intensity profiles of this model to the massive protostar G35.2-0.74N, including SOFIA-FORCAST observations at 30 and 40 microns. Good agreement is achieved, showing that a massive, ~ 30 Msun, protostar is forming from a high surface density core, ~ 1g/cm^2, via relatively ordered collapse and accretion, which is driving powerful bipolar outflows. This result supports the Core Accretion theory which predicts that massive stars form similarly to their low-mass counterparts. A full model grid covering the expected environmental conditions under which massive stars form will be further developed.