I will present a study of core-collapse supernovae (CCSNe) based on a one-dimensional, Lagrangian model that solves the hydrodynamics and radiation transport in an expanding ejecta. The models are compared with observations to constrain the physical properties of the progenitor star, such as radius and mixing of radioactive nickel synthesized during the explosion. In particular, I will present hydrodynamic and stellar evolution models for the type IIb SN 2011dh and for the type Ib iPTF13bvn. In both cases we were able to provide a self-consistent model to explain the pre-SN photometry, the chemical composition and the SN properties assuming that the progenitor stars were part of binary interacting systems. The disappearance of the putative progenitor of SN 2011dh last year confirmed our hydrodynamical modelling of this object. Recent near-UV HST observations at the position of SN 2011dh showed the presence of a blue point source with properties compatible with our predicted companion star. If confirmed, the companion star would already be dominant in the UV–optical regime, so it would readily provide a unique opportunity to perform a detailed study of its properties. In the case of iPTF13bvn, if our binary models are correct, which can be tested with future HST observations, this would provide the first robust identification of a progenitor system for a Type Ib SN.