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(Abridged) We aim at linking the dynamical and radiative properties of theremnant of SN 1987A to the geometrical and physical characteristics of theparent aspherical SN explosion and to the internal structure of its progenitorstar. We performed 3D hydrodynamic simulations which describe the long-termevolution of SN 1987A from the onset of the SN to the full-fledged remnant atthe age of 50 years, accounting for the pre-SN structure of the progenitorstar. The simulations include all physical processes relevant for the complexphases of SN evolution and for the interaction of the SNR with the highlyinhomogeneous ambient environment around SN 1987A. From the simulations, wesynthesize observables to be compared with observations. By comparing the modelresults with observations, we constrained the initial SN anisotropy causingDoppler shifts observed in emission lines of heavy elements from ejecta, andleading to the remnant evolution observed in the X-ray band in the last 30years. In particular, we found that the high mixing of ejecta unveiled by highredshifts and broadenings of [FeII] and $^{44}$Ti lines require a highlyasymmetric SN explosion channeling a significant fraction of energy along anaxis almost lying in the plane of the central equatorial ring around SN 1987A,roughly along the line-of-sight but with an offset of 40 deg, with the lobepropagating away from the observer slightly more energetic than the other. Wefound unambiguously that the observed distribution of ejecta and the dynamicaland radiative properties of the SNR can be best reproduced if the structure ofthe progenitor star was that of a blue supergiant resulted from the merging oftwo massive stars.

Hydrodynamic simulations unravel the progenitor-supernova-remnant connection in SN 1987A