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

D. N. Aguilera·D. Blaschke·H. Grigorian
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Abstract

We study the consequences of antineutrino trapping in hot quark matter for quark star configurations with possible diquark condensation. Due to the conditions of charge neutrality and beta-equilibrium the flavor asymmetry increases with the number density of trapped antineutrinos such that above a critical value of the antineutrino chemical potential of 30 MeV diquark condensation is inhibited. When the quark star cools a two-phase structure occurs: a superconducting quark matter core surrounded by a shell of normal quark matter. Below the critical temperature of about 1 MeV, the antineutrino mean free path becomes larger than the thickness of the normal quark matter shell so that they get untrapped within a sudden process. By comparing the masses of configurations with the same baryon number we estimate that the release of energy due to the antineutrino untrapping transition can be in the range of 10^{51} to 10^{52} erg.

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D. N. Aguilera, D. Blaschke, H. Grigorian. 2003-11-04. Energy release due to antineutrino untrapping and diquark condensation in hot quark star evolution. https://doi.org/10.1051/0004-6361%3A20031742

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