Spin and Center of mass comparison between the PN approach and the asymptotic formulation

Abstract

In this work we analyse the similarities and differences between the equations of motion for the center of mass and intrinsic angular momentum for isolated sources of gravitational radiation obtained by two different formulations. One approach is based on the asymptotic formulation of the GR whereas the other relies on Post- Newtonian methods. Several conclusions are obtained which could be useful for further developments in both approaches.

References in corpus (3)

• GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2
• GW170814: A Three-Detector Observation of Gravitational Waves from a Binary Black Hole Coalescence
• Using Full Information When Computing Modes of Post-Newtonian Waveforms From Inspiralling Compact Binaries in Circular Orbit

Cited by in corpus (12)

• The RIT binary black hole simulations catalog
• The Poincaré and BMS flux-balance laws with application to binary systems
• The Third RIT binary black hole simulations catalog
• Flux-balance equations for linear momentum and center-of-mass position of self-gravitating post-Newtonian systems
• Multipole expansion of gravitational waves: memory effects and Bondi aspects
• Analyzing Gravitational Waves with General Relativity
• Gravitational radiation reaction for compact binary systems at the fourth-and-a-half post-Newtonian order
• A relativistic center of mass in general relativity
• Gravitational waves from quasielliptic compact binaries in scalar-tensor theory to one-and-a-half post-Newtonian order
• Numerical evolution of the center of mass and angular momentum for binaries black holes
• Final velocity and radiated energy in numerical simulations of binary black holes
• Gravitational radiation reaction for compact binary systems at the fourth-and-a-half post-Newtonian order in harmonic coordinates