  We consider the gamma-ray burst of 1997 February 28 (GRB 970228) within the
ElectroMagnetic Black Hole (EMBH) model. We first determine the value of the
two free parameters that characterize energetically the GRB phenomenon in the
EMBH model, that is to say the dyadosphere energy, $E_{dya}=5.1\times10^{52}$
ergs, and the baryonic remnant mass $M_{B}$ in units of $E_{dya}$,
$B=M_{B}c^{2}/E_{dya}=3.0\times10^{-3}$. Having in this way estimated the
energy emitted during the beam-target phase, we evaluate the role of the
InterStellar Medium (ISM) number density (n$_{ISM}$) and of the ratio ${\cal
R}$ between the effective emitting area and the total surface area of the GRB
source, in reproducing the observed profiles of the GRB 970228 prompt emission
and X-ray (2-10 keV energy band) afterglow. The importance of the ISM
distribution three-dimensional treatment around the central black hole is also
stressed in this analysis.
