  In this work, we have investigated a novel aspect of black hole (BH)
formation during the collapse of a self-gravitating configuration. The exact
solution of the Einstein field equations is obtained in a model-independent way
by considering a parametrization of the expansion scalar ($\Theta$) in the
background of spherically symmetric space-time geometry governed by the FLRW
metric. Smooth matching of the interior solution with the Schwarzschild
exterior metric across the boundary hypersurface of the star, together with the
condition that the mass function $m(t,r)$ is equal to Schwarzschild mass $M$,
is used to obtain all the physical and geometrical parameters in terms of the
stellar mass. The four known massive stars namely $R136a3$, $Melnick$, $R136c$,
and $R136b$ with their known astrophysical data (mass, radius, and present age)
are used to study the physics of the model both numerically and graphically. We
demonstrate that the formation of the apparent horizon occurs earlier than the
singular state that is, the model of massive stars would inevitably lead to the
formation of a BH as their end state. We have conducted an analysis indicating
that the lifespans of massive stars are closely related to their respective
masses. Our findings demonstrate that more massive stars exhibit considerably
shorter lifespans in comparison to their lighter counterparts. Thus, the
presented model corresponds to the evolutionary stages of astrophysical stellar
objects and theoretically predicts their possible lifespan. We have also shown
that our model satisfies the energy conditions and stability requirements via
Herrera's cracking method.
