We address the problem of crystallization, melting and evaporation of dust particles in disks around YSOs. This problem has attracted much interest in recent years since it is one important feature which gives considerable insight into evolutionary processes in such disks that is accesible to observations with the new generation of large telescopes. Shock waves seems to be the mechanism able to explain the formation of crystalline silicates found in chondrites, long-period comets, and disks around YSOs (Jones et al. 2000, Protostars and Planets IV, 927; Scott and Krot 2004, ApJ in press). We propose a new energy source of gas dynamics shocks based on gravitational perturbations excited by a companion object, i.e., a giant planet or a companion star. We carry out a parameterization of the wave dynamics and of the dust heating in the shock front that predicts the melting and/or evaporation of silicates in bound orbital ranges determined by the companion orbital semiaxis. We obtain that the gravitational perturbations of the companion would generate shock waves able to process dust particles at ~ 1-8 AU depending on the central star and disk physical parameters as well as on the companion parameters (Sterzik and Parisi 2006 submitted to $A\&A$). We especulate that the precense and abundance of crystalline and amorphus silicate grains in young binary systems (young brown dwarfs, T-Tauri stars, and Herbig AeBe stars) are determined by this process. Current infrared observations are just approaching the necessary precision to test this hypothesis.