Adjust the electron fraction (Ye) based on rest mass density (rho). More...
#include <ParameterizedDeleptonization.hpp>
Classes | |
| struct | ElectronFractionAtHighDensity |
| Electron fraction of material when the rest mass density is above HighDensityScale. More... | |
| struct | ElectronFractionAtLowDensity |
| Electron fraction of material when the rest mass density is below LowDensityScale. More... | |
| struct | ElectronFractionCorrectionScale |
| Electron fraction correction term. The larger this value, the higher the Ye of matter at densities between LowDensityScale and HighDensityScale. More... | |
| struct | Enable |
| Use an analytic expression vs rest mass density profile. More... | |
| struct | HighDensityScale |
| Density near the center of the supernova at bounce, above which the central Ye is assumed. More... | |
| struct | LowDensityScale |
| Density near the Silicon-Oxygen interface, below which the lower Ye is assumed. More... | |
Public Types | |
| using | options = implementation defined |
| using | return_tags = implementation defined |
| using | argument_tags = implementation defined |
Public Member Functions | |
| 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={}) | |
| ParameterizedDeleptonization (const ParameterizedDeleptonization &)=default | |
| ParameterizedDeleptonization & | operator= (const ParameterizedDeleptonization &)=default |
| ParameterizedDeleptonization (ParameterizedDeleptonization &&)=default | |
| ParameterizedDeleptonization & | operator= (ParameterizedDeleptonization &&)=default |
| void | pup (PUP::er &p) |
| 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 |
Static Public Attributes | |
| static constexpr Options::String | help |
Friends | |
| bool | operator== (const ParameterizedDeleptonization &lhs, const ParameterizedDeleptonization &rhs) |
Adjust the electron fraction (Ye) based on rest mass density (rho).
Based on [126] 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.
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staticconstexpr |