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It was recently demonstrated that the eruption of V1309 Sco was a result of amerger of the components of a cool contact binary. We computed a set ofevolutionary models of the detached binaries with different initial parametersto compare it with pre-burst observations of V1309 Sco. The models are based onour recently developed evolutionary model of the formation of cool contactbinaries. The best agreement with observations was obtained for binaries withinitial masses of 1.8-2.0 solar masses and initial periods of 2.5-3.1 d. Theevolution of these binaries consists of three phases: at first the binary isdetached and both components lose mass and angular momentum through amagnetized wind. This takes almost two thirds of the total evolutionarylifetime. The remaining third is spent in a semi-detached configuration of theAlgol-type, following the Roche-lobe overflow by the initially more massivecomponent. When the other component leaves the main sequence and moves towardthe giant branch, a contact configuration is formed for a short time, followedby the coalescence of both components.

Evolution of the progenitor binary of V1309 Scorpii before merger