  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.
