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SpECTRE
v2026.09.05
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Items related to solving the gravitational self-force of a gravitating body in a Kerr background. More...
Namespaces | |
| namespace | Tags |
| Tags for the GrSelfForce system. | |
Classes | |
| struct | FirstOrderSystem |
| Gravitational self-force of a small gravitating body in a Kerr background. More... | |
| struct | Fluxes |
| Fluxes \(F^i\) for the gravitational self-force system. More... | |
| struct | ModifyBoundaryData |
| Adds or subtracts the singular field to/from the received data on element boundaries. More... | |
| struct | Sources |
| Source terms for the gravitational self-force system. More... | |
Typedefs | |
| using | GradTensorType |
| We're working with 4D tensors to represent the 10 independent components we're solving for, but we only take 2D spatial derivatives, so we define these mixed-dimension tensors for gradients and fluxes. | |
| using | FluxTensorType |
| We're working with 4D tensors to represent the 10 independent components we're solving for, but we only take 2D spatial derivatives, so we define these mixed-dimension tensors for gradients and fluxes. | |
Functions | |
| void | fluxes (gsl::not_null< FluxTensorType * > flux, const tnsr::I< ComplexDataVector, 2 > &alpha, const GradTensorType &field_gradient) |
| The first-order flux \(F^i=\alpha^i \partial_i \Psi_m\). | |
| void | fluxes_on_face (gsl::not_null< FluxTensorType * > flux, const tnsr::I< ComplexDataVector, 2 > &alpha, const tnsr::I< DataVector, 2 > &face_normal_vector, const tnsr::aa< ComplexDataVector, 3 > &field) |
| The first-order flux on an element face \(F^i=\alpha^i n_i \Psi_m\). | |
| void | add_sources (gsl::not_null< tnsr::aa< ComplexDataVector, 3 > * > source, const tnsr::aaBB< ComplexDataVector, 3 > &beta, const tnsr::aaBB< ComplexDataVector, 3 > &gamma_rstar, const tnsr::aaBB< ComplexDataVector, 3 > &gamma_theta, const tnsr::aa< ComplexDataVector, 3 > &field, const GradTensorType &field_gradient) |
| The source term \(\beta_{ab}^{cd} (\Psi_m)_{cd} + \gamma_{iab}^{cd}
\partial_i (\Psi_m)_{cd}\). | |
Items related to solving the gravitational self-force of a gravitating body in a Kerr background.
We're working with 4D tensors to represent the 10 independent components we're solving for, but we only take 2D spatial derivatives, so we define these mixed-dimension tensors for gradients and fluxes.
We're working with 4D tensors to represent the 10 independent components we're solving for, but we only take 2D spatial derivatives, so we define these mixed-dimension tensors for gradients and fluxes.