Mass accretion from the CMZ inwards. Top: mass contained in the cylindrical volume R < 150 pc as a function of time for the CHEM_MHD and CHEM_HD simulations. Bottom: inflow rate into the same volume, which represents the inflow from the CMZ ring inwards. Similarly to Fig. 22, we show the time averaged inflow rate (black lines) as well as the non-averaged one (grey lines). The inflow is zero in the HD simulation, while it is significant in the MHD simulation. The spikes in the top panel for the HD simulation are caused by orbiting clouds that temporarily enter the R = 150 pc region, but that eventually leave (M at the end of the HD simulation is zero as can be seen in the top panel). Inflow at these scales is mainly driven by the magnetorota-tional instability (Sect. 7).