Multi-domain spectral method for Kerr spacetimes: a hyperboloidal Teukolsky m-mode solver for self-force computations
Abstract
We solve the frequency-domain, m-mode Teukolsky equation for the spin-weight s=−2 Weyl scalar ψ4 sourced by a point mass on a circular, equatorial orbit around a Kerr black hole. The equation is posed on hyperboloidal slices that reach the event horizon and future null infinity, so that the physical (retarded) solution is selected by regularity alone, without imposing radiation conditions. The particle is treated with the m-mode puncture/effective-source scheme, and the resulting two-dimensional elliptic problem is solved with a four-domain pseudo-spectral method in which the equatorial symmetry is broken and handled by an even/odd decomposition of the field. We test the method for orbital radius r0=10M and spins up to |a|/M=0.9, covering prograde and retrograde orbits. The energy fluxes to infinity agree with independent Black Hole Perturbation Toolkit results to ∼10−7 for the dominant modes and to better than 2×10−5 for all modes up to m=20 at moderate resolutions. The static m=0 mode requires no special treatment.
Related
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BibTeX
@misc{cownden2026multidomain,
title = {{Multi-domain spectral method for Kerr spacetimes: a hyperboloidal Teukolsky $m$-mode solver for self-force computations}},
author = {Brad Cownden and Rodrigo Panosso Macedo and Christiana Pantelidou and Samuel D. Upton and Barry Wardell},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.03870},
eprint = {2611.03870},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.03870},
note = {CC BY-NC-SA 4.0},
}
RIS
TY - UNPB
TI - Multi-domain spectral method for Kerr spacetimes: a hyperboloidal Teukolsky m-mode solver for self-force computations
AU - Brad Cownden
AU - Rodrigo Panosso Macedo
AU - Christiana Pantelidou
AU - Samuel D. Upton
AU - Barry Wardell
PY - 2026
DA - 2026/11/02
PB - arXiv
DO - 10.48550/arxiv.2611.03870
UR - https://arxiv.org/abs/2611.03870
AB - We solve the frequency-domain, m-mode Teukolsky equation for the spin-weight s=−2 Weyl scalar ψ_4 sourced by a point mass on a circular, equatorial orbit around a Kerr black hole. The equation is posed on hyperboloidal slices that reach the event horizon and future null infinity, so that the physical (retarded) solution is selected by regularity alone, without imposing radiation conditions. The particle is treated with the m-mode puncture/effective-source scheme, and the resulting two-dimensional elliptic problem is solved with a four-domain pseudo-spectral method in which the equatorial symmetry is broken and handled by an even/odd decomposition of the field. We test the method for orbital radius r_0=10M and spins up to |a|/M=0.9, covering prograde and retrograde orbits. The energy fluxes to infinity agree with independent Black Hole Perturbation Toolkit results to ∼10^−7 for the dominant modes and to better than 2×10^−5 for all modes up to m=20 at moderate resolutions. The static m=0 mode requires no special treatment.
ER -