Irradiation Environment for Planets in Habitable Zone

This thesis explores the complexities of cosmic habitability, investigates the influence of M-dwarf stars, the role of high-energy radiation and water, as well as the likelihood of water loss during different planetary phases. Specific attention is given to the habitability of Proxima b and TRAPPIST-1’s planets and the factors governing their habitable zones. Chapter 5 presents original research. Initially, primary conditions are considered to identify target exoplanets. Subsequently, detailed evolutionary models are created. Factors such as luminosity, age, and the inner distance of planets are then analyzed, considering two different models and four different amounts of fluxes that planets could receive in various phases of their lives. Following this, the investigation shifts to determining the duration that planets spend outside the habitable zone before transitioning into it and makes approximate about the amount of water mass planets have lost in those duration comparing to TRAPPIST-1 and Proxima b. This provides valuable insights into the temporal aspects of habitability. These investigations offer a nuanced understanding of the interplay between stellar characteristics, planetary conditions, and the temporal dynamics of habitable zones. This thesis contributes to existing knowledge and sets the stage for future exploration in the captivating field of cosmic habitability.