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

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