Density profiles of the radiative non-isothermal models with M(τ) = 0. The vertical lines mark the position of the sonic radius for each model. As the UV emission becomes stronger, the accreting gas becomes supersonic at larger radial distances from the SMBH, while the density becomes higher for x ≲ 0.2. These trends apply only to models M₂ and M₃, while model M₁, having an arbitrary θ₀ and weaker UV emission, becomes supersonic at a much larger distance from the SMBH and achieves a much higher central densities than models M₂ and M₃.