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We present a new semi-analytic model of the formation of the first stars. Ourmethod takes dark matter halo merger trees (including 3-dimensional spatialinformation) from cosmological N-body simulations as input and applies analyticprescriptions to compute both the Population III (Pop III) and metal-enrichedstar formation histories. We have developed a novel method to accuratelycompute the major feedback processes affecting Pop III star formation: H$_2$photodissociation from Lyman-Werner (LW) radiation, suppression of starformation due to inhomogeneous reionization, and metal enrichment viasupernovae winds. Our method utilizes a grid-based approach relying on fastFourier transforms (FFTs) to rapidly track the LW intensity, ionizationfraction, and metallicity in 3-dimensions throughout the simulation box. Wepresent simulations for a wide range of astrophysical model parameters from$z\approx 30-6$. Initially long-range LW feedback and local metal enrichmentand reionization feedback dominate. However, for $z \lesssim 15$ we find thatthe star formation rate density (SFRD) of Pop III stars is impacted by thecombination of external metal enrichment (metals from one halo polluting otherpristine halos) and inhomogeneous reionization. We find that the interplay ofthese processes is particularly important for the Pop III SFRD at $z \lesssim10$. Reionization feedback delays star formation long enough for metal bubblesto reach halos that would otherwise form Pop III stars. Including these effectscan lead to more than an order of magnitude decrease in the Pop III SFRD at$z=6$ compared to LW feedback alone.

Self-consistent Semi-analytic Modeling of Feedback During Primordial Star Formation and Reionization