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In this work we investigate protoneutron star properties within a modifiedversion of the quark coupling model (QMC) that incorporates a omega-rhointeraction plus kaon condensed matter at finite temperature. Fixed entropy andtrapped neutrinos are taken into account. Our results are compared with theones obtained with the GM1 parametrization of the non-linear Walecka model forsimilar values of the symmetry energy slope. Contrary to GM1, within the QMCthe formation of low mass black-holes during cooling are not probable. It isshown that the evolution of the protoneutron star may include the melting ofthe kaon condensate driven by the neutrino diffusion, followed by the formationof a second condensate after cooling. The signature of this complex proccesscould be a neutrino signal followed by a gamma ray burst. We have seen thatboth models can, in general, describe very massive stars.

Effects of the symmetry energy on the kaon condensates in the QMC Model