Investigation into the possibility of the formation of an accretion disc around the inner binary when the tertiary fills its Roche lobe. The figure shows the ratios of the apocentre distance of the inner two stars to the expected circularisation radius of the inflowing material, that is a_in(1 + e_in)/R_circ. The dashed lines represent the distribution for the subset of systems for which we expect the mass transfer from the tertiary towards the inner binary to occur in a stable manner. The distribution is normalised to unity.