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 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 Maxwell-Lorentz without self-interactions: Conservation of energy and momentum

2022 ◽  
Author(s):  
Jonathan Gratus
Keyword(s):  
Reaction Force ◽  
Radiation Reaction ◽  
Point Particle ◽  
Energy Tensor ◽  
Stress Energy Tensor ◽  
Conservation Of Energy ◽  
Stress Energy ◽  
Energy And Momentum ◽  
Charged Point ◽  
Radiation Reaction Force

Abstract Since a classical charged point particle radiates energy and momentum it is argued that there must be a radiation reaction force. Here we present an action for the Maxwell-Lorentz without self interactions model, where each particle only responds to the fields of the other charged particles. The corresponding stress-energy tensor automatically conserves energy and momentum in Minkowski and other appropriate spacetimes. Hence there is no need for any radiation reaction.

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.

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