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We study the consequences of antineutrino trapping in hot quark matter forquark star configurations with possible diquark condensation. Due to theconditions of charge neutrality and beta-equilibrium the flavor asymmetryincreases with the number density of trapped antineutrinos such that above acritical value of the antineutrino chemical potential of 30 MeV diquarkcondensation is inhibited. When the quark star cools a two-phase structureoccurs: a superconducting quark matter core surrounded by a shell of normalquark matter. Below the critical temperature of about 1 MeV, the antineutrinomean free path becomes larger than the thickness of the normal quark mattershell so that they get untrapped within a sudden process. By comparing themasses of configurations with the same baryon number we estimate that therelease of energy due to the antineutrino untrapping transition can be in therange of 10^{51} to 10^{52} erg.Comment: 7 pages, 5 figures, uses aa.cls (included), numerical results  updated, reference added, minor text modification

Energy release due to antineutrino untrapping and diquark condensation in hot quark star evolution