Dependency of the accretion rates on the smoothing length and opacities for simulations with the highest available resolution as depicted in Fig. 8. Left: averaged accretion rates from 5 to 15 orbits, for down to and our three different opacity values. Simulation runs with have such a shallow potential that the horseshoe flows, which penetrate down to approximately also interfere with the envelope cooling process. Right: accretion rates with Bell and Lin opacities, with 1 (=solar), 0.1, and 0.01% dust opacities, as well as a run with Malygin opacities and ɛ=0.01%. Simulation runs with have been shown in Fig. 8 to be sufficiently resolved. We therefore interpret the seen downwards trend of Ṁ with as real (red dashed line), even if runs with are only at the verge of fulfilling our convergence criterion.