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We present results of general relativistic simulations of collapsingsupermassive stars with and without rotation using the two-dimensional generalrelativistic numerical code Nada, which solves the Einstein equations writtenin the BSSN formalism and the general relativistic hydrodynamics equations withhigh resolution shock capturing schemes. These numerical simulations use anequation of state which includes effects of gas pressure, and in a tabulatedform those associated with radiation and the electron-positron pairs. We alsotake into account the effect of thermonuclear energy released by hydrogen andhelium burning. We find that objects with a mass of 5x10^{5} solar mass and aninitial metallicity greater than Z_{CNO}~0.007 do explode if non-rotating,while the threshold metallicity for an explosion is reduced to Z_{CNO}~0.001for objects uniformly rotating. The critical initial metallicity for athermonuclear explosion increases for stars with mass ~10^{6} solar mass. Forthose stars that do not explode we follow the evolution beyond the phase ofblack hole formation. We compute the neutrino energy loss rates due to severalprocesses that may be relevant during the gravitational collapse of theseobjects. The peak luminosities of neutrinos and antineutrinos of all flavorsfor models collapsing to a BH are ~10^{55} erg/s. The total radiated energy inneutrinos varies between ~10^{56} ergs for models collapsing to a BH, and~10^{45}-10^{46} ergs for models exploding.

Relativistic collapse and explosion of rotating supermassive stars with thermonuclear effects