Modeling Disks Around Massive Protostars

Details Modeling Disks Around Massive Protostars Modeling Disks Around Massive Protostars

Jan 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21725808c&link_type=abstract

American Astronomical Society, AAS Meeting #217, #258.08; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

While the process of massive star formation is uncertain, recent radiation hydrodynamical models suggest that massive stars could form through accretion. As part of this process, it is suggested that a massive protostellar disk could be formed around the protostar. Driven by this possibility, we explore the potential signatures of the existence of such disks. We thus have constructed and present a self-consistent model of a high-mass protostellar disk. In this case, we apply the disk to the well-studied region NGC 7538IRS9. In this model, we solve for the spatial structure of the temperature, density, and radiation field. With these inputs, we solve for the chemistry throughout the disk, including CO, CS, HCO+, H2O, OH, and C2H2. We then create simulated observations at different transitions and source inclinations. When compared with actual data, radiation from these four molecules provide potential constraints about the existence, as well as the structure and orientation of a disk.

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