  In course of the consolidation of nucleon (neutron) spacing inside a compact
star, two key factors are expected to come into play side by side: the lack of
self-stabilization against shutting into black hole (BH) and forthcoming phase
transition - color deconfinement and QCD-vacuum reconstruction - within the
nuclear matter the star is composed of. These phenomena bring the star to
evolve in the quite different (opposite) ways and should be taken into account
at once, as the gravitational compression is considered. Under the above
transition, which is expected to occur within any supermassive neutron star
(NS), the hadronic-phase (HPh) vacuum - a coherent state of gluon- and chiral
$q\bar q$-condensates - turns, first near the star center, into the "empty"
(perturbation) subhadronic-phase (SHPh) one and, thus, pre-existing (very high)
vacuum pressure falls there down rather abruptly; as a result, the "cold" star
starts collapsing almost freely into the new vacuum. If the stellar mass is
sufficiently large, then this implosion is shown to result in an enormous
heating within the star central domain (up to a temperature about 100-200 MeV
or, maybe, even higher), what makes the pressure from within to grow up,
predominantly due to degeneracy breaking and multiple $q\bar q$-pair
production. Thus, a "flaming wall" could arise, which withstands the further
collapsing and brings the star off the irrevocable shutting into BH. Instead,
the star either forms a transient quasi-steady state (just the case of
relatively low star mass) and, losing its mass, evolves gradually into the
"normal" steady NS, or is doomed for self-liquidation in full (at higher
masses).
