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The recently discovered exoplanets in binary or higher-order multiple stellarsystems sparked a new interest in the study of proto-planetary discs in stellaraggregations. Here we focus on disc solids, as they make up the reservoir outof which exoplanets are assembled and dominate (sub-)millimetre discobservations. These observations suggest that discs in binary systems arefainter and smaller than in isolated systems. In addition, disc dust sizes areconsistent with tidal truncation only if they orbit very eccentric binaries. Ina previous study we showed that the presence of a stellar companion hastens theradial migration of solids, shortening disc lifetime and challenging planetformation. In this paper we confront our theoretical and numerical results withobservations: disc dust fluxes and sizes from our models are computed at ALMAwavelengths and compared with Taurus and $\rho$ Ophiuchus data. A generalagreement between theory and observations is found. In particular, we show thatthe dust disc sizes are generally smaller than the binary truncation radius dueto the combined effect of grain growth and radial drift: therefore, small discsizes do not require implausibly high eccentricities to be explained.Furthermore, the observed binary discs are compatible within $1\sigma$ with aquadratic flux-radius correlation similar to that found for single-star discsand show a close match with the models. However, the observational sample ofresolved binary discs is still small and additional data are required to drawmore robust conclusions on the flux-radius correlation and how it depends onthe binary properties.

monthly notices of the royal astronomical society

On dust evolution in planet-forming discs in binary systems. II --  Comparison with Taurus and $\rho$ Ophiuchus (sub-)millimetre observations:  discs in binaries have small dust sizes