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Many stars are in binaries or higher-order multiple stellar systems. Althoughin recent years a large number of binaries have been proven to host exoplanets,how planet formation proceeds in multiple stellar systems has not been studiedmuch yet from the theoretical standpoint. In this paper we focus on theevolution of the dust grains in planet-forming discs in binaries. We take intoaccount the dynamics of gas and dust in discs around each component of a binarysystem under the hypothesis that the evolution of the circumprimary and thecircumsecondary discs is independent. It is known from previous studies thatthe secular evolution of the gas in binary discs is hastened due to the tidalinteractions with their hosting stars. Here we prove that binarity affects dustdynamics too, possibly in a more dramatic way than the gas. In particular, thepresence of a stellar companion significantly reduces the amount of solidsretained in binary discs because of a faster, more efficient radial drift,ultimately shortening their lifetime. We prove that how rapidly discs dispersedepends both on the binary separation, with discs in wider binaries livinglonger, and on the disc viscosity. Although the less-viscous discs lose highamounts of solids in the earliest stages of their evolution, they aredissipated slowly, while those with higher viscosities show an oppositebehaviour. The faster radial migration of dust in binary discs has a strikingimpact on planet formation, which seems to be inhibited in this hostileenvironment, unless other disc substructures halt radial drift further in. Weconclude that if planetesimal formation were viable in binary discs, thisprocess would take place on very short time scales.

On dust evolution in planet-forming discs in binary systems. I -- Theoretical and numerical modelling: radial drift is faster in binary discs