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Following the recently established "Binary-driven HyperNova" (BdHN) paradigm,we here interpret GRB 970828 in terms of the four episodes typical of such amodel. The "Episode 1", up to 40 s after the trigger time t_0, with a timevarying thermal emission and a total energy of E_{iso,1st} = 2.60 x 10^{53}erg, is interpreted as due to the onset of an hyper-critical accretion processonto a companion neutron star, triggered by the companion star, an FeCO coreapproaching a SN explosion. The "Episode 2", observed up t_0+90 s, isinterpreted as a canonical gamma ray burst, with an energy of E^{e^+e^-}_{tot}= 1.60 x 10^{53} erg, a baryon load of B = 7 x 10^{-3} and a bulk Lorentzfactor at transparency of \Gamma = 142.5. From this Episode 2, we infer thatthe GRB exploded in an environment with a large average particle density <n>\approx 10^3 particles/cm^3 and dense clouds characterized by typicaldimensions of (4 \div 8) x 10^{14} cm and \delta n / n ~ 10. The "Episode 3" isidentified from t_0+90 s all the way up to 10^{5-6} s: despite the paucity ofthe early X-ray data, typical in the BATSE, pre-Swift era, we find extremelysignificant data points in the late X-ray afterglow emission of GRB 970828,which corresponds to the ones observed in all BdHNe sources. The "Episode 4",related to the Supernova emission, does not appear to be observable in thissource, due to the presence of darkening from the large density of the GRBenvironment, also inferred from the analysis of the Episode 2.

Induced Gravitational Collapse in the BATSE era: the case of GRB 970828