Stars are complex objects involving multi-dimensional processes like convection, rotation and magnetic fields. Ideally, we would like to model stars with three-dimensional (3D) magneto-hydrodynamic (MHD) simulations but it is unfortunately not feasible to simulate their entire evolution in 3D. Stars, including massive stars, have thus mostly been modelled in 1D assuming spherical symmetry. Theoretical prescriptions are used to determine the 1D (time- and spherically-averaged) effects of the multi-D processes listed above into the 1D models. This has been quite successful over the past 50 years or so. The continuously improving observational constraints, however, have highlighted key deficiencies of the present 1D models. In particular asteroseismic constraints cannot be reproduced with stellar models including standard prescriptions of convection and rotation. With the increase in computing power with time, we now have the power to complement observational constraints with constraints from 3D (M)HD simulations of stellar interiors. In this talk, I will first give a brief introduction to 1D stellar evolution modelling and review some of its successes. I will then introduce a framework to develop synergy between 3D and 1D simulations of convection, the so-called RA-ILES framework. I will present recent results obtained by applying this framework to convective boundary mixing, which is one of the most important uncertainties in the evolution of stars of all masses. I will also discuss the topic of angular momentum transport and the related chemical mixing in stars. In this case, it is harder to use 3D simulations but we can use nucleosynthesis to complement other observational constraints. I will end the talk with a summary and outlook.