Fig. 9

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.
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