Tracing chemical evolution of high-mass star-forming regions

Abstract

High-mass star-forming regions are critical environments for understanding the chemical evolution of the interstellar medium (ISM) and the life cycle of Giant Molecular Clouds (GMCs). These star-forming regions undergo rapid and dynamic chemical evolution shaped by UV radiation field, feedback from stellar winds, ionization from cosmic rays, etc. These environments lead to the generation of rich chemical regions, including the synthesis of complex organic molecules. In this work, we use high-resolution MHD simulations for high-mass star formation and post-process it with the rate-equation-based gas-grain code, Saptarsy, to trace the evolution of various molecules as the star-forming region evolves. The recent improvements in the code mean it can deal with gas phase, gas-grain, and dust surface reactions using a multi-layered dust model.