A Fortran ('08) and python code that solves Teukolsky equation for the linearly perturbed Newman-Penrose scalar Psi4 about a Kerr black hole. The code also directly reconstructs the linear spacetime metric in outgoing radiation gauge from the linearized Newman-Penrose scalar Psi_4, and then solves the equations of motion for the second order Psi_4. The code evolves fields in the time domain, and spatial derivatives are evaluated using pseudo-spectral methods. For more information about the code and the formalism we use see the papers listed under Citation.

Look under Releases for the latest stable version of this code.

Runtime parameters are configured in the setup.py file.

• mpmath: http://mpmath.org/

• FFTW: http://fftw.org

• OpenMP (this is optional): https://www.openmp.org/

I have successfully compiled the code with gfortran (version 9) and ifort (version 17).

Feel free to contact me if you have any questions. Under docs/ there is a Documentation.md file which goes over how you can install the code, and how to read out data.

A Mathematica notebook that contains the equations of motion (as described in the code paper listed under Citation) in coordinate form can be found here.

We do not make use of the Kinnersley tetrad in this code. Instead, we make use of a rotation of that tetrad, which is described in more detail in Appendix C of arXiv:2010.00162 (see the bibtex citation at the end of this README; a copy of the oringal preprint form of this paper can be found under the docs directory). The upshot of this transformation is that at future null infinity, the real and imaginary parts of the Weyl scalar Psi4 limit to twice the second time derivative of the plus and cross polarizations of the metric perturbation at future null infinity, (not half those quantities, as is the case for the traditionally used Kinnersley tetrad). That is, the R.H.S. of Eq. (16) of arXiv:2010.00162 should be multiplied by 4.

I use pyqtgraph-graph derived software (see here) to visualize the data, which are saved as csv files.

There is a zenodo link at the top of this README, if you would like to directly cite the code.

If you use this code, please cite the following two papers, which describe the algorithm and methods in detail:

@article{Ripley:2020xby,
    author = "Ripley, Justin L. and Loutrel, Nicholas and Giorgi, Elena and Pretorius, Frans",
    title = "{Numerical computation of second order vacuum perturbations of Kerr black holes}",
    eprint = "2010.00162",
    archivePrefix = "arXiv",
    primaryClass = "gr-qc",
    doi = "10.1103/PhysRevD.103.104018",
    journal = "Phys. Rev. D",
    volume = "103",
    pages = "104018",
    year = "2021"
}

and

@article{Loutrel:2020wbw,
    author = "Loutrel, Nicholas and Ripley, Justin L. and Giorgi, Elena and Pretorius, Frans",
    title = "{Second Order Perturbations of Kerr Black Holes: Reconstruction of the Metric}",
    eprint = "2008.11770",
    archivePrefix = "arXiv",
    primaryClass = "gr-qc",
    doi = "10.1103/PhysRevD.103.104017",
    journal = "Phys. Rev. D",
    volume = "103",
    number = "10",
    pages = "104017",
    year = "2021"
}

A copy of both of these papers (in preprint form) can be found under the docs directory.

• June 2023: I have added one new IO option that was not present in the original code: there is now a write_sphere_coefs option in the setup.py file, which allows you to save to file the spherical harmonic components of the code output at each radial point. Thanks to Jaime Redondo-Yuste for catching a bug in this addition to the code.

• Oct 2022: A few bugs were introduced to the code in commits made after the publication of arXiv:2008:11770 and arXiv:2010.00162. I have reverted the code to close to its original form, so that running this code should give allow you to reproduce the figures in arXiv:2010.00162. Discrepancies in the code output were found by Hengrui Zhu. If you are interested in the newer experimental version of the code, please let me know.

For questions please contact Justin Ripley: ripley [at] illinois [dot] edu