PDR Astrochemical Models of Massive Star Formation

We present astrochemical models of a massive protostar forming from a 60 solar mass core in the context of the Turbulent Core Model (McKee & Tan 2003). An evolutionary sequence is studied via snapshots of the core, including infall envelope, disk, outflow cavity and protostellar properties for protostellar masses of 1, 2, 4, 8, 12, 16 and 24 solar masses, taken from the Zhang & Tan (2018) model grid. We utilize the DALI code (Bruderer et al. 2012) to calculate radiative transfer of UV photons, especially in the FUV regime that create Photodissociation Regions (PDRs). A gas-grain chemical network is calculated, reponding to the radiation field and calculated gas temperature. We examine the abundances of various species, especially containing C and O, at various locations in the core and discuss observable signatures for various components, such as infall envelope, disk and outflow.