Abhay G. Shah

Extreme-mass-ratio inspiral corrections to the angular velocity and redshift factor of a mass in circular orbit about a Kerr black hole

This is the first of two papers on computing the self-force in a radiation gauge for a particle moving in circular, equatorial orbit about a Kerr black hole. In the EMRI (extreme-mass-ratio inspiral) framework, with mode-sum renormalization, we compute the renormalized value of the quantity

Gravitational Self-force in a Radiation Gauge

h_{\alpha\beta}u^\alpha u^\beta

Gravitational Self-Force Correction to the Innermost Stable Circular Equatorial Orbit of a Kerr Black Hole

, gauge-invariant under gauge transformations generated by a helically symmetric gauge vector; and we find the related order

Finding high-order analytic post-Newtonian parameters from a high-precision numerical self-force calculation

\frak{m}

Conservative, gravitational self-force for a particle in circular orbit around a Schwarzschild black hole in a radiation gauge

correction to the particles angular velocity at fixed renormalized redshift (and to its redshift at fixed angular velocity). The radiative part of the perturbed metric is constructed from the Hertz potential which is extracted from the Weyl scalar by an algebraic inversion\cite{sf2}. We then write the spin-weighted spheroidal harmonics as a sum over spin-weighted spherical harmonics and use mode-sum renormalization to find the renormalization coefficients by matching a series in

Metric perturbations produced by eccentric equatorial orbits around a Kerr black hole

L=\ell+1/2

Linear-in-mass-ratio contribution to spin precession and tidal invariants in Schwarzschild spacetime at very high post-Newtonian order

to the large-

Gravitational-wave flux for a particle orbiting a Kerr black hole to 20th post-Newtonian order: A numerical approach

L

Factorization and resummation: A new paradigm to improve gravitational wave amplitudes

behavior of the expression for

Self-force from reconstructed metric perturbations: Numerical implementation in Schwarzschild spacetime

H := \frac12 h_{\alpha\beta}u^\alpha u^\beta