Abstract

We calculate the potential contributions of the motion of binary mass systems in gravity to the fifth post–Newtonian order ab initio using coupling and velocity expansions within an effective field theory approach based on Feynman amplitudes starting with harmonic coordinates and using dimensional regularization. Furthermore, the singular and logarithmic tail contributions are calculated. We also consider the non–local tail contributions. Further steps towards the complete calculation are discussed. We calculate all but the rational O(ν2) contributions to the bound state energy for circular motion and periastron advance K(Eˆ,j). Comparisons are given to results in the literature.

Highlights

  • The measurement of gravitational wave signals from merging black holes and neutron stars [1] has been a recent milestone in astrophysics

  • SNRGR,bulk is the same as the general relativity bulk action SGR,bulk from Eq (20), but without the potential contributions to the metric. Both VNZ and the effective stress–energy tensor T μν are fixed by requiring that the non–relativistic general relativity (NRGR) action produces the same predictions as the asymptotic expansion of the full theory

  • We have presented the 5PN potential contributions to the Hamiltonian of binary motion in gravity starting form the harmonic gauge and a part of the 5PN tail term

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Summary

Introduction

The measurement of gravitational wave signals from merging black holes and neutron stars [1] has been a recent milestone in astrophysics. In binary Hamiltonian dynamics the level of the 4th post–Newtonian (PN) order has been fully understood and agreeing results have been obtained using a variety of different computation techniques in quite a series of gauges which lead to identical predictions in all key observables [3,4,5,6,7,8,9] It has been shown by applying canonical transformations [9], that all descriptions are dynamically equivalent. In the case of the tail terms one first applies the multi–pole expansion valid for the far zone [3,13,15,25,27,31,32,33,34,35,36,37,38,39] to the respective post–Newtonian order and applies EFT methods to calculate their contribution, cf [40]. As well we present longer formulae, which are used in the present calculation

The potential contributions to the Hamiltonian
Remarks on the tail term
The pole-free Hamiltonian at 5PN
Canonical transformation to EOB
The non-local terms
Periastron advance: local terms
The π2 contributions
Comparison to the other contributions to the tail terms
Conclusions
B The eccentricity expansion of the non–local terms
C The contour integral for the Delaunay variable ir

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