# Título:  Decaimento eletrofraco da matéria de quarks no interior das estrelas de nêutrons

Resumo:

In this work we study the phase transition from hadronic to quark matter in neutron stars and  proto-neutron stars. The transition begins with the deconfinement of hadrons, which is driven by strong interactions, and is followed by the weak interaction decay of quarks until quark matter reaches chemical equilibrium. We calculate the rate of all the relevant weak interaction processes in hot and dense quark matter and solve the Boltzmann equation in order to derive the decay timescale and the neutrino emissivity.  We have systematically taken into account the effect of strong interactions perturbatively to order $\alpha_c$ and the effect of finite temperature and strange quark mass.

We show that the transition raises the temperature of quark matter up to 60-70 MeV and chemical equilibrium is attained in a timescale of a nanosecond.  We find that the neutrino emissivity per baryon is very large, 10^{10} - 10^{12} MeV/ s. We analyze the astrophysical consequences of the results.

### Orientador: Prof. Dr. German Lugones

Titulares

• Orientador: Prof. Dr. German Lugones - UFABC
• Prof. Dr. Laura Paulucci Marinho - UFABC
• Prof. Dr. Ernesto Kemp - UNICAMP

Suplentes

• Prof. Dr. Alex Gomes Dias - UFABC
• Prof. Dr. Orlando Luis Goulart Peres - UNICAMP

### PUBLICAÇÕES RECENTES

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