scholarly journals Optimizing the third-and-a-half post-Newtonian gravitational radiation-reaction force for numerical simulations

2003 ◽  
Vol 68 (8) ◽  
Author(s):  
Guillaume Faye ◽  
Gerhard Schäfer
Keyword(s):  
Numerical Simulations ◽  
Gravitational Radiation ◽  
Reaction Force ◽  
Radiation Reaction ◽  
The Third ◽  
Radiation Reaction Force

scholarly journals Reaction force of gravitational radiation in an effective-one-body theory based on the post-Minkowskian approximation

2021 ◽  
Vol 81 (9) ◽  
Author(s):  
Manman Sun ◽  
Shuai Chen ◽  
Xiaokai He ◽  
Jiliang Jing
Keyword(s):  
Gravitational Wave ◽  
Gravitational Radiation ◽  
Loss Rate ◽  
Signal To Noise Ratio ◽  
Reaction Force ◽  
Radiation Reaction ◽  
High Signal ◽  
Effective Metric ◽  
Body Theory ◽  
Radiation Reaction Force

AbstractEffective-one-body (EOB) theory based on the post-Newtonian (PN) approximation presented by Buonanno and Damour plays an important role in the analysis of gravitational wave signals. Based on the post-Minkowskian (PM) approximation, Damour introduced another novel EOB theory which will lead to theoretically improved versions of the EOB conservative dynamics and might be useful in the upcoming era of high signal-to-noise-ratio gravitational-wave observations. Using the 2PM effective metric obtained by us recently, in this paper we study the radiation reaction force experienced by the particle with the help of the energy-loss-rate, which is an important step to construct the EOB theory based on the PM approximation.

scholarly journals A Poynting theorem formulation for the gravitational wave stress pseudo tensor

2021 ◽  
pp. 2142003
Author(s):  
Steven A. Balbus
Keyword(s):  
Gravitational Wave ◽  
Gravitational Radiation ◽  
Reaction Force ◽  
Radiation Reaction ◽  
Conservation Equation ◽  
Stress Energy ◽  
Exact Agreement ◽  
Poynting Theorem ◽  
Gravitational Contribution ◽  
Radiation Reaction Force

A very simple and physical derivation of the conservation equation for the propagation of gravitational radiation is presented. The formulation is exact. The result takes the readily recognisable and intuitive form of a Poynting-style equation, in which the outward propagation of stress energy is directly related to the volumetric equivalent of a radiation reaction force acting back upon the sources, including the purely gravitational contribution to the sources. Upon averaging, the emergent pseudo tensor for the gravitational radiation is in exact agreement with that found by much more labour-intensive methods.

scholarly journals Constructing a Mass‐Current Radiation‐Reaction Force for Numerical Simulations

1999 ◽  
Vol 525 (2) ◽  
pp. 935-949 ◽  
Author(s):  
Luciano Rezzolla ◽  
Masaru Shibata ◽  
Hideki Asada ◽  
Thomas W. Baumgarte ◽  
Stuart L. Shapiro
Keyword(s):  
Numerical Simulations ◽  
Reaction Force ◽  
Radiation Reaction ◽  
Radiation Reaction Force

Radiation-reaction force on a moving mirror

1993 ◽  
Vol 3 (11) ◽  
pp. 2151-2159 ◽  
Author(s):  
Claudia Eberlein
Keyword(s):  
Reaction Force ◽  
Radiation Reaction ◽  
Radiation Reaction Force

The two-body problem: an effective-one-body approach

2018 ◽  
Author(s):  
Nathalie Deruelle ◽  
Jean-Philippe Uzan
Keyword(s):  
Body Problem ◽  
Equations Of Motion ◽  
Reaction Force ◽  
Kerr Black Hole ◽  
Radiation Reaction ◽  
Spherically Symmetric ◽  
Geodesic Motion ◽  
Two Body Problem ◽  
Symmetric Spacetime ◽  
Radiation Reaction Force

This chapter presents the basics of the ‘effective-one-body’ approach to the two-body problem in general relativity. It also shows that the 2PN equations of motion can be mapped. This can be done by means of an appropriate canonical transformation, to a geodesic motion in a static, spherically symmetric spacetime, thus considerably simplifying the dynamics. Then, including the 2.5PN radiation reaction force in the (resummed) equations of motion, this chapter provides the waveform during the inspiral, merger, and ringdown phases of the coalescence of two non-spinning black holes into a final Kerr black hole. The chapter also comments on the current developments of this approach, which is instrumental in building the libraries of waveform templates that are needed to analyze the data collected by the current gravitational wave detectors.

scholarly journals Guiding-centre transformation of the radiation–reaction force in a non-uniform magnetic field

2015 ◽  
Vol 81 (5) ◽  
Author(s):  
E. Hirvijoki ◽  
J. Decker ◽  
A. J. Brizard ◽  
O. Embréus
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Uniform Magnetic Field ◽  
Reaction Force ◽  
Charged Particles ◽  
Collision Operator ◽  
Radiation Reaction ◽  
Transform Method ◽  
Lie Transform ◽  
Radiation Reaction Force

In this paper, we present the guiding-centre transformation of the radiation–reaction force of a classical point charge travelling in a non-uniform magnetic field. The transformation is valid as long as the gyroradius of the charged particles is much smaller than the magnetic field non-uniformity length scale, so that the guiding-centre Lie-transform method is applicable. Elimination of the gyromotion time scale from the radiation–reaction force is obtained with the Poisson-bracket formalism originally introduced by Brizard (Phys. Plasmas, vol. 11, 2004, 4429–4438), where it was used to eliminate the fast gyromotion from the Fokker–Planck collision operator. The formalism presented here is applicable to the motion of charged particles in planetary magnetic fields as well as in magnetic confinement fusion plasmas, where the corresponding so-called synchrotron radiation can be detected. Applications of the guiding-centre radiation–reaction force include tracing of charged particle orbits in complex magnetic fields as well as the kinetic description of plasma when the loss of energy and momentum due to radiation plays an important role, e.g. for runaway-electron dynamics in tokamaks.

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