Astronomy and Astrophysics – Astrophysics – High Energy Astrophysical Phenomena
Scientific paper
2010-06-04
Astronomy and Astrophysics
Astrophysics
High Energy Astrophysical Phenomena
11 pages, 2 figures
Scientific paper
Along with compacting baryon (neutron) spacing in a neutron star (NS), two very important factors come into play side by side: the lack of the NS gravitational self-stabilization against shutting to black hole (BH) and the phase transition - color deconfinement and QCD-vacuum reconstruction - within the nuclear matter the NS is composed of. That is why both phenomena should be taken into account at once, as the gravitational collapse is considered. Since, under the above transition, the hadronic-phase (HPh) vacuum (filled up with gluon- and chiral $q\bar q$-condensates) turns into the "empty" (perturbation) subhadronic-phase (SHPh) one and, thus, the formerly (very high) pressure falls down rather abruptly, the formerly cold nuclear medium starts imploding almost freely into the new vacuum. If the star mass is sufficiently large, then this implosion is shown to result in an enormous heating - up to the temperature about 100 MeV or, may be, even higher - and growth of the inner pressure due to degeneracy breaking and multiple $q\bar q$-pair production which withstands the gravitational compression (remind that the highest temperatures of supernovae bursts, as well as of the "normal" NS, are, at least, of one order lower). As a consequence, a "flaming wall" is, most probably, emerged on the way of further collapsing which prevents the NS to evolve towards the BH horizon appearance. At the same time, it could give rise to the most powerful GRBs produced by some very distant (young) stars.
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