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We combined hydrodynamical simulations of planet-disk interactions with dustevolution models that include coagulation and fragmentation of dust grains overa large range of radii and derived observational properties using radiativetransfer calculations. We studied the role of the snow line in the survival ofthe inner disk of transition disks. Inside the snow line, the lack of icemantles in dust particles decreases the sticking efficiency between grains. Asa consequence, particles fragment at lower collision velocities than in regionsbeyond the snow line. This effect allows small particles to be maintained forup to a few Myrs within the first astronomical unit. These particles areclosely coupled to the gas and do not drift significantly with respect to thegas. For lower mass planets (1$M_{\rm{Jup}}$), the pre-transition appearancecan be maintained even longer because dust still trickles through the gapcreated by the planet, moves invisibly and quickly in the form of relativelylarge grains through the gap, and becomes visible again as it fragments andgets slowed down inside of the snow line. The global study of dust evolution ofa disk with an embedded planet, including the changes of the dust aerodynamicsnear the snow line, can explain the concentration of millimetre-sized particlesin the outer disk and the survival of the dust in the inner disk if a largedust trap is present in the outer disk. This behaviour solves the conundrum ofthe combination of both near-infrared excess and ring-like millimetre emissionobserved in several transition disks.

A tunnel and a traffic jam: How transition disks maintain a detectable warm dust component despite the presence of a large planet-carved gap