Structure of an accretion disc around a ULXP. For very high mass accretion rates, the inner parts of the disc (inside the spherization radius R_sph shown here) enter the super-Eddington accretion regime. Inside R_sph the thin disc model is not applicable. Mass loss in a wind is shown by blue arrows. The accretion column, where most of the energy is released, is shown by yellow cones, and the red wavy lines refer to the radiation of the column that may affect the inner disc pressure balance. The red vertical line marks the effective boundary between the disc and the magnetosphere at R_in.