The Crab system, composed of a bright pulsar wind nebula (PWN) powered by the young energetic central pulsar \crabpulsar,
has been observed across the electromagnetic spectrum for decades of investigation. Its emission in the gamma-ray band has challenged our understanding
of the radiation and particle acceleration processes at play for such systems. In addition to the steady-state synchrotron emission from the PWN,
sporadic flares have been observed in the energy range from a few hundreds of MeV to a few GeV.

By analysing available Fermi-LAT data across a fourteen-year-long monitoring, we study the energy-dependence and time-variability of the high-energy flares.
Using a sample of flaring epochs derived by Bayesian-block analysis, we investigate the short and longer term effects
on the steady-state emission of the system, while attempting characterising the significant flares in terms of their spectral evolution with time.
Finally, we discuss the extent to which our latest results can place constraints on particle acceleration in the pulsar wind.