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Add documentation of past evolution
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joaorebelo-megum committed Aug 27, 2024
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14 changes: 14 additions & 0 deletions docs/References.bib
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Expand Up @@ -444,6 +444,20 @@ @article{Buchman:2012dw
year = "2012"
}

@article{Buonanno2005xu,
author = "Buonanno, Alessandra and Chen, Yanbei and Damour, Thibault",
title = "{Transition from inspiral to plunge in precessing binaries of
spinning black holes}",
eprint = "gr-qc/0508067",
archivePrefix = "arXiv",
doi = "10.1103/PhysRevD.74.104005",
journal = "Phys. Rev. D",
volume = "74",
pages = "104005",
year = "2006",
url = "https://doi.org/10.1103/PhysRevD.74.104005"
}

@article{Casoni2012,
author = {Casoni, E. and Peraire, J. and Huerta, A.},
title = {One-dimensional shock-capturing for high-order discontinuous
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Expand Up @@ -556,6 +556,29 @@ struct BinaryWithGravitationalWavesVariables
*
* \warning The class is still being worked on. The Solver was not tested yet,
* for now we still see a very slow convergence.
*
* To be able to calculate equations \f$\eqref{eq:retarded_term}\f$ and
* \f$\eqref{eq:integral_term}\f$ we need to look into the past history
* of the binary at least up to the time were the generated wave can reach the
* furthest point on the grid. To do so we must evolve the binary backward in
* time. Because we are only looking into the inspiral phase we can follow a
* simple Hamiltonian evolution computed in Post-Newtonian orders. The
* equations to be solved are
*
* \f{equation}{
* \frac{d X^i}{d t}=\frac{\partial H}{\partial P_i}
* \f}
*
* and
*
* \f{equation}{
* \frac{d P_i}{d t}=-\frac{\partial H}{\partial X^i}+F_i,
* \f}
*
* where $H$ is the Post-Newtonian Hamiltonian, $X^i$ is the separation
* vector between the two particles, $P_i$ is the momentum of one particle
* in the center of mass frame and $F_i$ is the radiation-reaction flux term.
* The Post-Newtonian Hamiltonian is given in \cite Buonanno2005xu.
*/
class BinaryWithGravitationalWaves
: public elliptic::analytic_data::Background,
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