Author ORCID Identifier

https://orcid.org/0009-0005-2363-9274

Date of Award

Spring 6-10-2026

Document Type

Thesis (Undergraduate)

Department

Physics and Astronomy

First Advisor

Elisabeth Newton

Abstract

Transmission spectroscopy of hot Jupiters enables mass and atmospheric composition measurements, providing insight into population dynamics and evolution when other methods are hindered by stellar activity. To effectively plan observations and interpret transmission spectra, we must have a robust understanding of how atmospheres evolve over time. To that end, we present a suite of hot Jupiter transmission spectra models with ages ranging from 3 Myr to 11 Gyr. We incorporate the cooling and contraction of the planet, which impacts the atmospheric profile, and the evolution of the stellar UV spectrum, which moderates photodissociation and photoionization. Using PICASO,  VULCAN, and FastChem in conjunction with observed spectra, we demonstrate how hot Jupiter atmospheric structure and chemistry respond to evolving stellar and planetary properties. We identify the broad observational changes in hot Jupiter transmission spectra over time, finding that the host star's luminosity evolution over the course of its main sequence lifetime is the driving force behind atmospheric transformation. Finally, we simulate observations of two young hot Jupiters, demonstrating the capacity for ground-based constraints on planetary mass using optical transmission spectroscopy. This work will support future observations with current and upcoming missions like JWST, CHEOPS, and ARIEL.

Download

Share

COinS