Temperature is a fundamental quality of any object of astrophysical study, and has remained elusive in the case of gas-rich protoplanetary disks. In these disks, we are particularly interested in understanding the thermal structure all the way down to the midplane, where the temperature will affect substructure that we see in both the mm-continuum and gas, as well as determining when, where, and how planets will form. In this project, we are interested in setting the thermal stage for planet formation in gaseous disks. Thermal information, especially deep within the disk is difficult to obtain, and requires observations of multiple temperature and surface density tracers. We utilized a suite of CO observations and a key HD flux measurement in combination with RAC2D thermo-chemical simulation to understand the 2D thermal structure of the gas-rich disk TW Hydra. We find that the final disk model must be warmer than previous estimates have predicted

Determining the thermal structure of gaseous protoplanetary disks: TW hydra

Macromolecular Chemistry: The Second Century

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ACS Spring 2020 National Meeting & Expo

The official archive and repository for all ACS Meetings & Expositions abstracts and select posters or presentations.