• Corpus ID: 231582913

Gravitational wave templates from Extreme Mass Ratio Inspirals

@inproceedings{Skoupy2021GravitationalWT,
  title={Gravitational wave templates from Extreme Mass Ratio Inspirals},
  author={Viktor Skoup'y and Georgios Lukes-Gerakopoulos Institute of Theoretical Physics and Faculty of Mathematics and Physics and Charles University and Prague and Czech Republic and Astronomical Institute of the Slovak Academy of Sciences},
  year={2021}
}
An extreme mass ratio inspiral takes place when a compact stellar object is inspiraling into a supermassive black hole due to gravitational radiation reaction. Gravitational waves (GWs) from this system can be calculated using the Teukolsky equation (TE). In our case, we compute the asymptotic GW fluxes of a spinning body orbiting a Kerr black hole by solving numerically the TE both in time and frequency domain. Our ultimate goal is to produce GW templates for space-based detectors such as LISA… 

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References

SHOWING 1-10 OF 19 REFERENCES
Gravitational wave snapshots of generic extreme mass ratio inspirals
Using black hole perturbation theory, we calculate the gravitational waves produced by test particles moving on bound geodesic orbits about rotating black holes. The orbits we consider are
Self-force and radiation reaction in general relativity.
TLDR
This review surveys the theory of gravitational self- force in curved spacetime and its application to the astrophysical inspiral problem, and highlights the way in which self-force calculations make a fruitful contact with other approaches to the two-body problem and help inform an accurate universal model of binary black hole inspirals, valid across all mass ratios.
A new gravitational wave generation algorithm for particle perturbations of the Kerr spacetime
We present a new approach to solve the 2+1 Teukolsky equation for gravitational perturbations of a Kerr black hole. Our approach relies on a new horizon penetrating, hyperboloidal foliation of Kerr
Laser Interferometer Space Antenna
Following the selection of The Gravitational Universe by ESA, and the successful flight of LISA Pathfinder, the LISA Consortium now proposes a 4 year mission in response to ESA's call for missions
Gravitational waves from a spinning particle in circular orbits around a rotating black hole.
TLDR
The post-Newtonian formula of the gravitational wave luminosity up to the order (v/c) 5 beyond the quadrupole formula including the linear order of particle spin is presented.
Periastron advance in spinning black hole binaries: comparing effective-one-body and Numerical Relativity
We compute the periastron advance using the effective-one-body formalism for binary black holes moving on quasicircular orbits and having spins collinear with the orbital angular momentum. We compare
Hamilton-Jacobi equation for spinning particles near black holes
A compact stellar-mass object inspiralling onto a massive black hole deviates from geodesic motion due to radiation-reaction forces as well as finite-size effects. Such post-geodesic deviations need
Spinning test body orbiting around a Schwarzschild black hole: Circular dynamics and gravitational-wave fluxes
We consider a spinning test-body in circular motion around a nonrotating black hole and analyze different prescriptions for the body's dynamics. We compare, for the first time, the
Factorization and resummation: A new paradigm to improve gravitational wave amplitudes
We introduce a new, resummed, analytical form of the post-Newtonian (PN), factorized, multipolar amplitude corrections $f_{\ell m}$ of the effective-one-body (EOB) gravitational waveform of spinning,
Celestial mechanics in Kerr spacetime
The dynamical parameters conventionally used to specify the orbit of a test particle in Kerr spacetime are the energy E, the axial component of the angular momentum, Lz, and Carter's constant Q.
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