Abstract
The gravitational waves emitted by binary systems with extreme mass ratios carry unique astrophysical information expected to be probed by the next generation of gravitational wave detectors such as LISA. The detection of these binaries rely on an accurate modeling of the gravitational self-force that drives their orbital evolution. Although the theoretical formalism to compute the self-force has been largely established, the mathematical tools needed to implement it are still under development, and the self-force computation remains an open problem. We present here a frequency-domain implementation of the particle-without-particle (PwP) technique previously developed for the computation of the scalar self-force – a helpful testbed for the gravitational self-force.
Highlights
Introduction and Motivation ExtremeMass-Ratio Inspirals (EMRIs) are one of the main sources of gravitational waves (GWs) for space-based detectors like the LISA mission
The challenge in modeling ExtremeMass-Ratio Inspirals (EMRIs) is to compute the perturbations generated by the stellar compact object (SCO) in the gravitational field of the massive black hole (MBH), and how these perturbations affect the motion of the SCO itself
In our simplified EMRI model, the SCO is a charged scalar particle, with charge q associated to a scalar field Φ, orbiting a non-rotating MBH with a fixed geometry, the Schwarzschild-Droste metric
Summary
Introduction and Motivation ExtremeMass-Ratio Inspirals (EMRIs) are one of the main sources of gravitational waves (GWs) for space-based detectors like the LISA mission. The challenge in modeling EMRIs is to compute the perturbations generated by the SCO in the (background) gravitational field of the MBH, and how these perturbations affect the motion of the SCO itself.
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