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Hot molecular cores (HMCs) are intermediate stages of high-mass starformation and are also known for their rich emission line spectra at (sub-)mmwavebands. The observed spectral feature of HMCs such as total number ofemission lines and associated line intensities are also found to vary withevolutionary stages. We developed various 3D models for HMCs guided by theevolutionary scenarios proposed by recent empirical and modeling studies. Wethen investigated the spatio-temporal variation of temperature and molecularabundances in HMCs by consistently coupling gas-grain chemical evolution withradiative transfer calculations. We explored the effects of varying physicalconditions on molecular abundances including density distribution andluminosity evolution of the central protostar(s). The time-dependenttemperature structure of the hot core models provides a realistic framework forinvestigating the spatial variation of ice mantle evaporation as a function ofevolutionary timescales. With increasing protostellar luminosity, the water iceevaporation font ($\sim$100K) expands and the spatial distribution of gas phaseabundances of these COMs also spreads out. We simulated the synthetic spectrafor these models at different evolutionary timescales to compare withobservations. A qualitative comparison of the simulated and observed spectrasuggests that these self-consistent hot core models can reproduce the notabletrends in hot core spectral variation within the typical hot core timescales of10$^{5}$ year. These models predict that the spatial distribution of variousemission line maps will also expand with evolutionary time. The modelpredictions can be compared with high resolution observation that can probescales of a few thousand AU in high-mass star forming regions such as fromALMA.[Abridged]

Evolution of complex organic molecules in hot molecular cores: Synthetic spectra at (sub-)mm wavebands