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| ParameterizedDeleptonization (bool enable, double high_density_scale, double low_density_scale, double electron_fraction_at_high_density, double electron_fraction_at_low_density, double electron_fraction_correction_scale, const Options::Context &context={}) |
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| ParameterizedDeleptonization (const ParameterizedDeleptonization &)=default |
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ParameterizedDeleptonization & | operator= (const ParameterizedDeleptonization &)=default |
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| ParameterizedDeleptonization (ParameterizedDeleptonization &&)=default |
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ParameterizedDeleptonization & | operator= (ParameterizedDeleptonization &&)=default |
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void | pup (PUP::er &p) |
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template<size_t ThermodynamicDim> |
| void | operator() (gsl::not_null< Scalar< DataVector > * > specific_internal_energy, gsl::not_null< Scalar< DataVector > * > electron_fraction, gsl::not_null< Scalar< DataVector > * > pressure, gsl::not_null< Scalar< DataVector > * > temperature, const Scalar< DataVector > &rest_mass_density, const EquationsOfState::EquationOfState< true, ThermodynamicDim > &equation_of_state) const |
Adjust the electron fraction (Ye) based on rest mass density (rho).
Based on [131] spherically symmetric Boltzmann calculations, during the collapse phase just before a core-collapse supernova, the electron fraction naturally follows the rest mass density. Intuitively, the higher the density, the more electrons are captured onto protons, leading to neutrino production. As these neutrinos diffuse out of the center of the collapsing star, the total number of leptons near center of the CCSN drops—the process of deleptonization.
https://iopscience.iop.org/article/10.1086/466517