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The evolution of single stars at low metallicity has attracted a largeinterest, while the effect of metallicity on binary evolution remains stillrelatively unexplored. We study the effect of metallicity on the number ofbinary systems that undergo different cases of mass transfer. We find thatbinaries at low metallicity are more likely to start transferring mass afterthe onset of central helium burning, often referred to as case C mass transfer.In other words, the donor star in a metal poor binary is more likely to haveformed a massive CO core before the onset of mass transfer.  At solar metallicity the range of initial binary separations that result incase C evolution is very small for massive stars, because they do not expandmuch after the ignition of helium and because mass loss from the system bystellar winds causes the orbit to widen, preventing the primary star to fillits Roche lobe. This effect is likely to have important consequences for themetallicity dependence of the formation rate of various objects through binaryevolution channels, such as long GRBs, double neutron stars and double whitedwarfs.

Binaries at Low Metallicity: ranges for case A, B and C mass transfer