How protostars, still actively accreting and highly embedded in their natal cores, grow their mass is still a greatly debated question. The High-resolution Accretion Disks of Embedded protoStars (HADES) simulations are a suite of simulations currently underway to investigate the accretion and outflow properties around protostars at high resolution. These simulations will push to resolve the the shocks and instabilities in the accretion region at sub-mAU scales. We plan to run several simulations for different magnetic field morphologies for both low- and high- mass protostars to investigate the role of magnetic fields on regulating the accretion. The current "pathfinder" suit of simulations includes non-ideal magneto-hydrodynamics, viscosity and a background potential. Future simulations will include radiation transfer, including ionizing radiation, self gravity and hydrogen chemistry. One of the key features of these simulations is the time-cadence outputs, at 20 minutes of physical time between each output. This degree of high time-cadence allows detailed investigations of variability, which is now observed in recombination lines in near- and mid-infrared emission lines. The simulations will be post-processed to predict the variability in these lines for different results. Due to the high data cadence, the simulations will produce a significant amount of data to be analysed to measure the variability of the gas flows throughout the domain and related observables.