Modelling reflected polarised light from close-in giant exoplanet WASP-96b using PolHEx (Polarisation of Hot Exoplanets)

TL;DR

This paper introduces the PolHEx code for modeling reflected flux and polarisation spectra of hot Jupiter exoplanets, incorporating atmospheric inhomogeneities and cloud particle properties to improve interpretation of observational data.

Contribution

The study develops a comprehensive modeling framework combining climate and cloud models to analyze polarised light from hot exoplanets, emphasizing the role of cloud composition and shape.

Findings

Cloud particle composition affects reflected flux and polarisation.

Orbital phase influences the spectra due to atmospheric inhomogeneities.

Particle shape impacts the reflected spectra and polarisation signals.

Abstract

We present the Polarisation of Hot Exoplanets (PolHEx) code for modelling the total flux (F) and degree of linear polarisation (P) of light spectra reflected by close-in, tidally locked exoplanets. We use the output from a global climate model (GCM) combined with a kinetic cloud model of hot Jupiter WASP-96b as a base to investigate effects of atmospheric longitudinal-latitudinal inhomogeneities on these spectra. We model F and P-spectra as functions of wavelength and planet orbital phase for various model atmospheres. We find different materials and sizes of cloud particles to impact the reflected flux F, and particularly the linear polarisation state P. A range of materials are used to form inhomogeneous mixed-material cloud particles (Al2O3, Fe2O3, Fe2SiO4, FeO, Fe, Mg2SiO4, MgO, MgSiO3, SiO2, SiO, TiO2), with Fe2O3, Fe, and FeO the most strongly absorbing species. The cloud particles near the relatively cool morning terminator are expected to have smaller average sizes and a narrower size distribution than those near the warmer evening terminator, which leads to different reflected spectra at the respective orbital phases .We also find differences in the spectra of F and P as functions of orbital phase for irregularly or spherically shaped cloud particles. This work highlights the importance of including polarisation in models and future observations of the reflection spectra of exoplanets.