A supplementary radiation-reaction force between two binaries

Abstract

Radiation-reaction forces originating from the emission of gravitational waves (GW) bring binaries to close proximity and are thus responsible for virtually all the mergers that we can observe in GW interferometers. We show that there exists a supplementary radiation-reaction force between two binaries interacting gravitationally, changing in particular the decay rate of the semimajor axis under the emission of GW. This new binary-binary force is in some settings of the same order-of-magnitude than the usual 2.5PN force for an isolated binary and presents some striking features such as a dependence on retarded time even in the post-Newtonian regime where all velocities are arbitrarily small. Using Effective Field Theory tools, we provide the expression of the force in generic configurations and show that it interpolates between several intuitive results in different limits. In particular, our formula generalizes the standard post-Newtonian estimates for radiation-reaction forces in $N$-body systems which are valid only in the limit where the GW wavelength goes to infinity.

Version accepted for publication in PRD

References in corpus (11)

• What is a globular cluster? An observational perspective
• Suppression of extreme orbital evolution in triple systems with short range forces
• Comparative statistics and origin of triple and quadruple stars
• Primordial Black Hole Dark Matter and the LIGO/Virgo observations
• The effect of matter structure on the gravitational waveform
• Circumbinary planets - why they are so likely to transit
• Detecting Kozai-Lidov imprints on the gravitational waves of intermediate-mass black holes in galactic nuclei
• Precession resonances in hierarchical triple systems
• About gravitational-wave generation by a three-body system
• Resonant capture in quadruple stellar systems
• Coupling of Dual Mass-Transferring White-Dwarf Binaries as a Variable Gravitational-Wave Emitter