| Abstract : | Our Solar System is believed to have been formed about 4.6 billion years ago in a cold molecular cloud. Its origin is still shrouded in mystery. The present state of planetary bodies, including our own Earth and the life on it are the direct result of various evolutionary processes that these objects have gone through during these many years. Isotopic studies of the solar system objects and other star and planet-forming regions allow us to reconstruct the past history of our own solar system. We can use isotopic ratios of H, C, O, and N as tools to understand the origin and evolutionary pathways of materials in star and planet-forming regions. To understand how isotopic ratios evolve spatially and temporally right from the molecular clouds to evolved sun-like planetary systems, we require consistent models coupled with sensitive observations. In this talk, I will discuss how isotopic ratio (D/H) helps us to constrain the planetary evolution processes by combining state-of-the-art astrochemical models coupled with radiative transfer and high-sensitive observations from the Atacama Large Millimeter/sub-millimeter Array (ALMA). Our work also suggests possibilities of carrying out such studies using future ground-based facilities such as the Square Kilometer Array (SKA). |
