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Pressure maxima are regions in protoplanetary disks where pebbles can betrapped because of the local absence of pressure gradient. These regions couldbe ideal places to form planetesimals or to isolate isotopic reservoirs.Observations of protoplanetary disks show that dusty rings structures arecommon, and pressure maxima are sometime invoked as a possible explanation. Inour Solar System, pressure bumps have been suggested as a possible mechanismfor separating reservoirs with different nucleosynthetic compositions. In thisletter we detail a mechanism by which pressure maxima form just inward thesnow-line in stratified disks. This mechanism does not need the presence of aplanet. Using a combination of analytical and numerical investigation weexplore the range of conditions for a pressure maximum to form inside thedead-zone and just inward the snow-line. When the vertically averaged $\alpha$is a decreasing function of surface density then the release of water vapor atthe snow-line lowers the sound velocity, and in turn, a pressure bump appears.This requires a constant inflow of icy pebbles with pebbles influx to gasinflux $>0.6$ for a power law disk with $1\%$ ice/gas ratio, and $>1.8$ for adisk with ice/gas ratio $\sim 0.3\%$. If these conditions are met, then aPressure-maximum appears just inward the snow-line due to a process couplingthe dead and active layers at the evaporation front. The pressure bump survivesas long as the icy pebble flux is high enough. The formation of the pressurebump is triggered by the drop of sound velocity inward the snow-line, due tothe release of water vapor. This mechanism is promising for isolating earlyreservoirs carrying different isotopic signatures in the Solar System and forpromoting dry planetesimal formation inward the snow-line, provided thevertically averaged description of a dead-zone is valid.

Forming pressure-traps at the snow-line to isolate isotopic reservoirs in the absence of a planet