On the nature of the ultrarelativistic prompt emission phase of GRB 190114C and GRB 180720B

A profound difference has occurred in the analysis of GRBs initially analyzed in the domain of gamma-ray astronomy with the Compton Gamma Ray Observatory and the BATSE Detector with the extension to X-ray astronomy and optical astronomy introduced by Beppo-SAX and the KEK and VLT optical observatory, followed by the AGILE, Fermi mission, Niels Gehrels SWIFT mission as well as HEHSS and MAGIC observations. An authentic ``Copernican revolution" has occurred in the transition from the traditional model of GRBs originating in a single star progenitor (collapsar) to GRBs with a binary progenitor composed of a CO core and a companion NS. We evidence from 24 SN observations related to GRBs that all of them, once analyzed with the general relativistic corrections, can be identified with I Bc Sn with a common value of the luminosity and common time of occurrence of the peak of the optical emission. This can be understood in terms of a precursor composed of a CO core and a binary NS companion. By contrast, the GRBs differ profoundly in their energetics which can be expressed in terms of 3 different classes of BDHNe: BDHN I, BDHN II, BDHN III, also originating from precursors composed of a CO core and a binary companion. It is pointed out how the analysis of these systems has profoundly modified the concept of the BH and the associated fundamental physics necessary for their description since the publication of ``Introducing the Black Hole" by Ruffini and Wheeler in 1971. At first, it is illustrated how the most radical change has occurred in the introduction of the effective BH charge, with an electric field only function of the BH dimensionless spin and a background magnetic field $B0$. This definitely indicates the abandonment of the Kerr--Newman solution in favour of the Kerr metric, for energy extraction processes in BH physics. We then enter in the detailed description of the ``seven Seals", the seven Episodes characterizing GRB 190114c and the associated SN 2019jrj. Based on the article by Aimuratov et al., in preparation.