) and Gases into Exoplanetary Atmospheres using 3-D Monte Carlo Simulations

Recent studies of the accretion process between exoplanets and their satellites provide new insights to the transfer of volatile elements, such as H₂O, CO₂, SO₂, SiO₂, Na, and K. In this study, we  present a new method of estimating the abundance and metallicity of SiO₂, in the atmospheres of gaseous exoplanets. Using 3-D weighted Monte Carlo simulations (SERPENS), and analytical models (DISHOOM) a model that provides the source rate of SiO₂, we can calculate the downward flux of particles and their interaction with the surrounding atmospheric conditions, where we can derive the abundance of SiO₂ relative to the background atmospheric composition. This allows us to track the evolution of orbiting neutral particles, and simulate their optical and infrared signatures (PROMETHEUS). Preliminary results of our models show that we may be able to detect approximately 1.6 parts per million (ppm) of SiO₂ in the atmospheres of these exoplanetary environments.