The phase variations of the Stokes components I (left), Q (middle), U (right), on the visible side of a planet as it rotates around its host star. The planet simulated here is viewed at an inclination angle of θ_incl = 30°, and has an oblateness of η = 0.3. It has an internal bottom-of-atmosphere temperature of T_int = 2000 K, a surface gravity ﹩\mathrm{log}g=4﹩, and solar metallicity. It is assumed to have a fine haze layer of optical thickness τ₁₀₀₀ = 1 and a lognormal size distribution of characteristic size r₀ = 0.1 μm at a characteristic width of σ₀ = 1.13, uniformly distributed between 1.0 and 0.5 bar.