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We examine the first phase of the core accretion model, namely the dustgrowth/fragmentation in binary systems. In our model, a gas and dust disk ispresent around the primary star and is perturbed by the secondary. We study theeffects of a secondary with/without eccentricity on the dust population todetermine what sizes the aggregates can reach and how that compares to the dustpopulation in disks around single stars.  We find that the secondary star has two effects on the dust population. 1.)The disk is truncated due to the presence of the secondary star and the maximummass of the particles is decreased in the lowered gas densities. This effect isdominant in the outer disk. 2.) The perturbation of the secondary pumps up theeccentricity of the gas disk, which in turn increases the relative velocitybetween the dust and the gas. Therefore the maximum particle sizes are furtherdecreased. The second effect of the secondary influences the entire disk.Coagulation is efficiently reduced even at the very inner parts of the disk.The average mass of the particles is reduced by four orders of magnitude (as aconsequence, the stopping time is reduced by one order of magnitude) in disksaround binary systems compared to dust in disks around single stars.

The first stages of planet formation in binary systems: How far can dust coagulation proceed?