ized by the high accretion rate.

Fig. \[fig:snap\_Ds\] shows the structure of the accretion flow at the end of the simulation. The whole [H[ii]{} ]{}bubble is shown within the large plotted area of Fig. \[fig:snap\_Ds\](a), while the central regions over $\sim 10^6$ AU and $\sim 10^5$ AU scales are enlarged in Figs. \[fig:snap\_Ds\](b) and \[fig:snap\_Ds\](c). Owing to the shadowing effect, we see in Fig. \[fig:snap\_Ds\](a) that the large horizontal neutral region cuts into the central part with the [H[ii]{} ]{}bubbles bound to the bipolar regions. Similarly to the case with disc radiation without shadowing effect (Sec. \[sec:disc\_rad\]), the gas within the bipolar [H[ii]{} ]{}bubbles flows outward and collides with the ambient neutral medium. The pressure equilibrium is approximately achieved throughout the simulation region, although the thermal pressure slightly decreases before the collision because the total pressure including the ram pressure is balanced. The size of the bipolar [H[ii]{} ]{}bubbles is much larger than in the former cases owing to the much higher luminosity $L \simeq 8L_{\mathrm{E}}$. Note that the injected radiation is super-Eddington only in the polar region with $\theta \gtrsim 50^\circ$.

Fig. \[fig:snap\_Ds\](b) shows that the gas inside the equatorial neutral region is almost at rest in the pressure equilibrium, while that on the surfaces is photoevaporated to join the ionized outflow. In Fig. \[fig:snap\_Ds\](c), where the structure over the scale of the Bondi radius is presented, the gas flows into the central sink through the equatorial neutral region. The density and pressure increase with decreasing $r$ for $r \lesssim r_{\mathrm{B}}$, as expected for the Bondi flow. As seen in Fig. \[fig:snap\_Ds\](b), the neutral gas is photoevaporated into the [H[ii]{} ]{}regions, where the acceleration by the radiation pressure is stronger than the gravitational pull owing to the super-Eddington fluxes in the polar directions. The accretion proceeds only through the solid angle co