Speaker
Description
We investigate the depletion radius of dark matter haloes by analyzing stacked mass flow rate (MFR) profiles derived from a large N-body cosmological simulation, focusing on its dependence on various halo properties. We find that the depletion radius is primarily determined by the conventional mass accretion rate, defined as the logarithmic growth rate of the virial mass with respect to the scale factor, consistent with similar previous findings. By analyzing the phase-space structure of haloes, we find that this dependence originates from the underestimated halo boundary definition and the crossing of non-smooth accretion material through this boundary. In contrast, the depletion radius associated with smooth accretion component shows high self-similarity and little dependence on the conventional accretion rate. These findings call for revisiting the connection between the spherical collapse model and cosmological simulations to fully understand this dependence.
