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We update the capabilities of the software instrument Modules for Experimentsin Stellar Astrophysics (MESA) and enhance its ease of use and availability.Our new approach to locating convective boundaries is consistent with thephysics of convection, and yields reliable values of the convective core massduring both hydrogen and helium burning phases. Stars with $M<8\,{\rm M_\odot}$become white dwarfs and cool to the point where the electrons are degenerateand the ions are strongly coupled, a realm now available to study with MESA dueto improved treatments of element diffusion, latent heat release, and blendingof equations of state. Studies of the final fates of massive stars are extendedin MESA by our addition of an approximate Riemann solver that captures shocksand conserves energy to high accuracy during dynamic epochs. We also introducea 1D capability for modeling the effects of Rayleigh-Taylor instabilities that,in combination with the coupling to a public version of the STELLA radiationtransfer instrument, creates new avenues for exploring Type II supernovaeproperties. These capabilities are exhibited with exploratory models ofpair-instability supernova, pulsational pair-instability supernova, and theformation of stellar mass black holes. The applicability of MESA is now widenedby the capability of importing multi-dimensional hydrodynamic models into MESA.We close by introducing software modules for handling floating point exceptionsand stellar model optimization, and four new software tools -- MESAWeb,MESA-Docker, pyMESA, and mesastar.org -- to enhance MESA's education andresearch impact.

Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions