**title** Asp Conference Series, Vol. **volume***, **year of Publication** **names of Editors**

This is a summary of the two talks presented at the Rome GRB meeting by C.L. Bianco and R. Ruffini. It is shown that by respecting the Relative Space-Time Transformation (RSTT) paradigm and the Interpretation of the Burst Structure (IBS) paradigm, important inferences are possible: a) in the new physics occurring in the energy sources of GRBs, b) on the structure of the bursts and c) on the composition of the interstellar matter surrounding the source. The understanding of new astrophysical phenomena is reached as soon as its energy source has been identified. This has been the case for pulsars (see Hewish et al., 1968) where the rotational energy of the neutron star was identified as the energy source (see e.g. Gold, 1968, 1969). Similarly, in binary X-ray sources the accretion process from a normal companion star in the deep potential well of a neutron star or a black hole has clearly pointed to the gravitational energy of the accreting matter as the basic energy source and consequently all the main features of the light curves of the sources have been clearly understood (Giacconi & Ruffini, 1978). In this spirit, our work in the field of Gamma-Ray Bursts (GRBs) has focused on identifing the energy extraction process from the black hole (Christodoulou & Ruffini, 1971) as the basic energy source for the GRB phenomenon. The distinguishing feature of this approach is a theoretically predicted source energetics all the way up to 1. formation of a " dyadosphere " , during the gravitational collapse leading to a black hole endowed with electromagnetic structure (EMBH) has been indicated as the initial boundary conditions of the GRB process (Ruffini, 1998; Preparata et al., 1998). Our model has been referred as " the EMBH model for GRBs " , although the EMBH physics only determines the initial boundary conditions of the GRB process by specifying the physical parameters and spatial extension of the neutral electron positron plasma originating the phenomenon. Traditionally, following the observations of the Vela (Strong, 1975) and CGRO 1 satellites, GRBs have been characterized by few parameters such as the fluence, the characteristic duration (T 90 or T 50) and the global time averaged