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- W3100114850 abstract "Several different processes could be changing the density in the core of a neutron star, leading to a departure from $beta$ equilibrium, quantified by the chemical potential difference $deltamuequivmu_n-mu_p-mu_e$. The evolution of this quantity is coupled to that of the star's interior temperature $T$ by two functions that quantify the rate at which neutrino-emitting reactions proceed: the net reaction rate (difference between $beta$ decay and capture rates), $Gamma_{rm net}(T,deltamu)$, and the total emissivity (total energy emission rate in the form of neutrinos and antineutrinos), $epsilon_{rm tot}(T,deltamu)$. Here, we present a simple and general relationship between these variables, ${partialepsilon_{rm tot}/partialdeltamu=3Gamma_{rm net}}$, and show that it holds even in the case of superfluid nucleons. This relation may simplify the numerical calculation of these quantities, including superfluid reduction factors." @default.
- W3100114850 created "2020-11-23" @default.
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- W3100114850 date "2006-10-11" @default.
- W3100114850 modified "2023-10-15" @default.
- W3100114850 title "Non-equilibrium beta processes in neutron stars: a relationship between the net reaction rate and the total emissivity of neutrinos" @default.
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- W3100114850 doi "https://doi.org/10.1111/j.1365-2966.2006.10851.x" @default.
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