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[Abridged] By appealing to a Quark-Nova (QN; the explosive transition of aneutron star to a quark star) in the wake of a core-collapse Supernovaexplosion of a massive star, we develop a unified model for long durationGamma-ray Bursts (LGRBs) and Fast Radio Bursts (FRBs). The time delay (years todecades) between the SN and the QN and, the fragmented nature (i.e. millions ofchunks) of the relativistic QN ejecta are key to yielding a robust LGRB engine.In our model, a LGRB light-curve exhibits the interaction of the fragmented QNejecta with a turbulent (i.e. filamentary and magnetically saturated) SN ejectawhich is shaped by its interaction with an underlying pulsar wind nebula (PWN).The afterglow is due to the interaction of the QN chunks, exiting the SNejecta, with the surrounding medium. Our model can fit BAT/XRT prompt andafterglow light-curves, simultaneously with their spectra, thus yielding theobserved properties of LGRBs (e.g. the Band function and the X-ray flares). Wefind that the Yonetoku law and the Amati law are not fundamental butphenomenological. FRBs result from coherent synchrotron emission when the QNchunks interact with non-turbulent weakly magnetized PWN-SN ejecta, whereconditions are prone to the Weibel instability. Magnetic field amplificationinduced by the Weibel instability sets the bunching length for electrons andpairs to radiate coherently. The resulting emission frequency, luminosity,duration and dispersion measure in our model are consistent with FRB data. Wefind a natural unification of high-energy burst phenomena from FRBs to LGRBsincluding X-ray Flashes and X-ray rich GRBs as well as Super-Luminous SNe. Wefind a possible connection between Ultra-High Energy Cosmic Rays and FRBs andpropose that a QN following a binary neutron star merger can yield a short GRB(SGRB) with fits to BAT/XRT light-curves.

A Quark-Nova in the wake of a core-collapse Supernova: a unifying model for long duration Gamma-Ray Bursts and Fast Radio Bursts