Exoplanets display a remarkable diversity in their physical and orbital properties across a wide range of parameter spaces. Correlations between planetary characteristics and host star properties provide crucial clues to their formation pathways and evolutionary histories. In this talk, I will present the results of my three thesis projects, all of which explore how exoplanet evolution is shaped by their host stars.

First, I will explore the population of giant exoplanets, which exhibit a broad range of orbital periods and eccentricities. Using stellar ages and metallicities from Gaia DR3, we identified intriguing correlations that point to the role of high-eccentricity migration and possible planet engulfment in shaping the observed population.

Second, I will focus on close-in, small transiting planets, whose radius distribution shows a pronounced bimodality between super-Earths (~1–2 R⊕) and sub-Neptunes (~2–4 R⊕), commonly referred to as the “evaporation valley” or “Fulton gap.” Recent studies indicate that the location and morphology of this valley depend on host star mass and spectral type. To investigate this, we developed a Bayesian forward-modeling framework that reproduces the observed planet population, constrains the initial planet distributions, and reveals a correlation between the median planet mass and host star mass.

Finally, I will explore atmospheric mass loss in close-in planets exposed to intense high-energy (XUV) irradiation from their host stars. By combining X-ray observations of host stars with planetary properties, we have computed mass-loss rates for 220 planets using the open-source hydrodynamic code ATES. We find that, under certain conditions, the mass-loss rates deviate significantly from the commonly assumed energy-limited prescription. Based on these results, we classify planets into three distinct theoretical photoevaporative regimes.

In addition, I will also summarize our group’s work on accretion and outflows in protoplanetary disks with JWST, led by Vinod and Shridharan.