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My thesis work aims to study the inter-relation between various physical andchemical conditions in a wide range of astrophysical environments. Our studiedregions range from the super-hot regions (i.e., nebular, photon-dominated, orphotodissociation regions, diffuse area, through which the lights of thebackground stars can reach us) to the super-cold regions (i.e., dense molecularclouds, proto-planetary disks, etc. where interstellar dust particles absorball background visible and ultra-violet lights). The chemical complexity of theinterstellar cloud gradually evolves due to the evolution in physicalconditions. The dense molecular clouds are the birth sites of star-formation,where a wide variety of complex organic molecules are observed. Dust particlesplay an essential role in the formation of these complex organic molecules.During the warm-up stage of a star-forming region, the molecules formed duringthe cold phase start to return to the gas phase by various thermal andnon-thermal evaporation processes. These complex molecules again freeze out tothe outer part of the proto-planetary disk during the further evolved stageaccording to their condensation temperature and form the so-called snow-lines.The binding energies of these molecules with the prevailing dust particles playa crucial role in determining the structural information of this disk. Thus thebinding energy of the molecules is vital to understand several critical aspectsof the star and planet formation processes. In this thesis, I will discuss thechemical complexity obtained in a wide range of the star-forming region andwhether this chemical complexity lead to biomolecules in space.

Physics And Chemistry Of Star Forming Region And Protoplanetary Disk