Ben Leather
@benleather.bsky.social
Marie Sklodowska-Curie Postdoctoral fellow, University of Southampton.
IG: @ben_leather
Web: http://benjaminleather.com
IG: @ben_leather
Web: http://benjaminleather.com
Now with added mint green hyperboloidal foliation.
November 25, 2024 at 11:52 PM
Now with added mint green hyperboloidal foliation.
6/ Next Steps
A similar Lorenz gauge metric reconstruction technique can now be implemented in Kerr. This, combined with the methods of this paper framework, paves the way for extending second-order GSF calculations to Kerr. I shall leave with you my nice Penrose diagram from the paper!
A similar Lorenz gauge metric reconstruction technique can now be implemented in Kerr. This, combined with the methods of this paper framework, paves the way for extending second-order GSF calculations to Kerr. I shall leave with you my nice Penrose diagram from the paper!
November 25, 2024 at 4:35 PM
6/ Next Steps
A similar Lorenz gauge metric reconstruction technique can now be implemented in Kerr. This, combined with the methods of this paper framework, paves the way for extending second-order GSF calculations to Kerr. I shall leave with you my nice Penrose diagram from the paper!
A similar Lorenz gauge metric reconstruction technique can now be implemented in Kerr. This, combined with the methods of this paper framework, paves the way for extending second-order GSF calculations to Kerr. I shall leave with you my nice Penrose diagram from the paper!
5/ Key Results
I reconstruct Lorenz gauge metric perturbations by gauge-transforming from the Regge-Wheeler gauge. This method calculates metric perturbations throughout the spacetime efficiently. It also enables accurate computations of fluxes, the Detweiler redshift, and self-force corrections.
I reconstruct Lorenz gauge metric perturbations by gauge-transforming from the Regge-Wheeler gauge. This method calculates metric perturbations throughout the spacetime efficiently. It also enables accurate computations of fluxes, the Detweiler redshift, and self-force corrections.
![A plot of the nonzero (conformal) BLS modes for ℓ=2 and m=2 throughout the spacetime that extends from the null-infinity (σ=0) to the horizon (σ=1). In this orbital configuration, the particle is located at σp=0.2. The field in Domain1, {D1}=[0,σp], is shown by the red curves, while the fields in Domain 2, {D2}=[σp,1], are shown by the blue curves.](https://cdn.bsky.app/img/feed_thumbnail/plain/did:plc:ctferuogbjc5psbjfmnpyr3c/bafkreidgu65qyiuiorwev5b2kvxbluw6anehbkzaxvz4mbywbcyozau5qe@jpeg)
November 25, 2024 at 4:35 PM
5/ Key Results
I reconstruct Lorenz gauge metric perturbations by gauge-transforming from the Regge-Wheeler gauge. This method calculates metric perturbations throughout the spacetime efficiently. It also enables accurate computations of fluxes, the Detweiler redshift, and self-force corrections.
I reconstruct Lorenz gauge metric perturbations by gauge-transforming from the Regge-Wheeler gauge. This method calculates metric perturbations throughout the spacetime efficiently. It also enables accurate computations of fluxes, the Detweiler redshift, and self-force corrections.
4/ Why Lorenz Gauge?
The Lorenz gauge simplifies the regularisation of singularities in GSF by ensuring isotropic singular behaviour. It also avoids divergences at null infinity and the horizon. Critically, this gauge aligns with the current second-order GSF framework.
The Lorenz gauge simplifies the regularisation of singularities in GSF by ensuring isotropic singular behaviour. It also avoids divergences at null infinity and the horizon. Critically, this gauge aligns with the current second-order GSF framework.
November 25, 2024 at 4:35 PM
4/ Why Lorenz Gauge?
The Lorenz gauge simplifies the regularisation of singularities in GSF by ensuring isotropic singular behaviour. It also avoids divergences at null infinity and the horizon. Critically, this gauge aligns with the current second-order GSF framework.
The Lorenz gauge simplifies the regularisation of singularities in GSF by ensuring isotropic singular behaviour. It also avoids divergences at null infinity and the horizon. Critically, this gauge aligns with the current second-order GSF framework.
3/ Novel Approach
I extend hyperboloidal slicing and spectral methods from a scalar toy model to full gravitational perturbations in the Lorenz gauge. These methods allow for compactified domain calculations that efficiently span the entire spacetime.
I extend hyperboloidal slicing and spectral methods from a scalar toy model to full gravitational perturbations in the Lorenz gauge. These methods allow for compactified domain calculations that efficiently span the entire spacetime.
November 25, 2024 at 4:35 PM
3/ Novel Approach
I extend hyperboloidal slicing and spectral methods from a scalar toy model to full gravitational perturbations in the Lorenz gauge. These methods allow for compactified domain calculations that efficiently span the entire spacetime.
I extend hyperboloidal slicing and spectral methods from a scalar toy model to full gravitational perturbations in the Lorenz gauge. These methods allow for compactified domain calculations that efficiently span the entire spacetime.
2/ How This Work Connects to EMRIs
Accurate GSF calculations require solving Einstein’s field equations for the smaller body’s perturbation of the spacetime. This work introduces a novel approach to calculating such a metric perturbation.
Accurate GSF calculations require solving Einstein’s field equations for the smaller body’s perturbation of the spacetime. This work introduces a novel approach to calculating such a metric perturbation.
November 25, 2024 at 4:35 PM
2/ How This Work Connects to EMRIs
Accurate GSF calculations require solving Einstein’s field equations for the smaller body’s perturbation of the spacetime. This work introduces a novel approach to calculating such a metric perturbation.
Accurate GSF calculations require solving Einstein’s field equations for the smaller body’s perturbation of the spacetime. This work introduces a novel approach to calculating such a metric perturbation.
1/ EMRIs and GSF
Extreme-mass-ratio inspirals (EMRIs) are key targets for future GW observatories like LISA. Their tiny mass ratios mean small corrections accumulate over thousands of orbits, making precise modelling essential. GSF theory is central to capturing these effects for accurate waveforms.
Extreme-mass-ratio inspirals (EMRIs) are key targets for future GW observatories like LISA. Their tiny mass ratios mean small corrections accumulate over thousands of orbits, making precise modelling essential. GSF theory is central to capturing these effects for accurate waveforms.
November 25, 2024 at 4:35 PM
1/ EMRIs and GSF
Extreme-mass-ratio inspirals (EMRIs) are key targets for future GW observatories like LISA. Their tiny mass ratios mean small corrections accumulate over thousands of orbits, making precise modelling essential. GSF theory is central to capturing these effects for accurate waveforms.
Extreme-mass-ratio inspirals (EMRIs) are key targets for future GW observatories like LISA. Their tiny mass ratios mean small corrections accumulate over thousands of orbits, making precise modelling essential. GSF theory is central to capturing these effects for accurate waveforms.