  To reconcile the observed unusual high luminosity of NuSTAR X-ray pulsations
from M82X-2 with the most extreme violation of the Eddington limit, and in view
that the persistent X-ray radiation from M82X-2 almost precludes the
possibility of common pulsars, we tackle the problem by the implications of
{\em microscopic theory of black hole} (MTBH). The preceding developments of
MTBH are proved to be quite fruitful for the physics of ultra-high energy (UHE)
cosmic-rays. Namely, replacing a central singularity by the infrastructures
inside event horizon, subject to certain rules, MTBH explains the origin of
ZeV-neutrinos which are of vital interest for the source of UHE-particles. The
M82X-2 is assumed to be a spinning intermediate mass black hole resided in
final stage of growth. As a corollary, the thermal blackbody X-ray emission
arisen due to the rotational kinetic energy of black hole escapes from event
horizon through the vista to outside world that detected as ultraluminous X-ray
pulsations. The M82X-2 indeed releases $\sim 99.6\%$ of its pulsed radiative
energy predominantly in the X-ray bandpass $0.3-30$ keV. We derive a pulse
profile and give a quantitative account of energetics and orbital parameters of
the semi-detached X-ray binary containing a primary accretor M82X-2 of inferred
mass $M\simeq 138.5-226\,M_{\odot}$ and secondary massive, $M_{2}> 48.3-
64.9\,M_{\odot}$, O/B-type donor star with radius of $R> 22.1-
25.7\,R_{\odot}$, respectively. We compute the torque added to M82X-2 per unit
mass of accreted matter which yields the measured spin-up rate.
