  In this paper, we explore the gravitational collapse of matter (dust) under
the effect of zero-point length $l_0$. During the gravitational collapse, we
have neglected the backreaction effect of the pre-Hawking radiation (in the
sense that it is small effect and cannot prevent the formation of apparent
horizon), then we recast the internal metric of a collapsing star as a closed
FRW universe for any spherically symmetric case and, finally, we obtain the
minimal value for the scale factor meaning that the particles never hit the
singularity. We argue that the object emerging at the end of the gravitational
collapse can be interpreted as Planck stars (black hole core) hidden inside the
event horizon of the black hole with radius proportional to
$(GMl_0^{2}/c^2)^{1/3}$. Quite interestingly, we found the same result for
radius of the Planck star using a free falling observer point of view. In
addition, we pointed out a correspondence between the modified Friedmann's
equations in loop quantum gravity and the modified Friedmann's equation in
string T-duality. In the end, we discuss two possibilities regarding the final
stage of the black hole. The first possibility is that we end up with a
Planck-size black hole remnants. The second possibility is that the inner core
can be unstable and, due to the quantum tunnelling effect, the spacetime can
undergo a black hole-to-white hole transition (a bouncing Planck star).
