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Content: For up to a few millions of years, pebbles must provide aquasi-steady inflow of solids from the outer parts of protoplanetary disks totheir inner regions. Aims: We wish to understand how a significant fraction ofthe pebbles grows into planetesimals instead of being lost to the host star.Methods:We examined analytically how the inward flow of pebbles is affected bythe snow line and under which conditions dust-rich (rocky) planetesimals form.When calculating the inward drift of solids that is due to gas drag, weincluded the back-reaction of the gas to the motion of the solids. Results: Weshow that in low-viscosity protoplanetary disks (with a monotonous surfacedensity similar to that of the minimum-mass solar nebula), the flow of pebblesdoes not usually reach the required surface density to form planetesimals bystreaming instability. We show, however, that if the pebble-to-gas-mass fluxexceeds a critical value, no steady solution can be found for the solid-to-gasratio. This is particularly important for low-viscosity disks (alpha < 10^(-3))where we show that inside of the snow line, silicate-dust grains ejected fromsublimating pebbles can accumulate, eventually leading to the formation ofdust-rich planetesimals directly by gravitational instability. Conclusions:This formation of dust-rich planetesimals may occur for extended periods oftime, while the snow line sweeps from several au to inside of 1 au. Therock-to-ice ratio may thus be globally significantly higher in planetesimalsand planets than in the central star.

Formation of dust-rich planetesimals from sublimated pebbles inside of the snow line