Abstract
In this paper, we study gravitational waves generated by binary systems within an extension of General Relativity which is described by the addition of quadratic in curvature tensor terms to the Einstein–Hilbert action. Treating quadratic gravity as an effective theory valid in the low energy/curvature regime, we argue that reliable calculations can be performed in the early inspiral phase, and furthermore, no flux of additional massive waves can be detected. We then compute the Yukawa suppressed dipole-like corrections to the post-Newtonian (PN) expansion of the standard waveform. By confronting these theoretical calculations with available experimental data, we constrain both unknown parameters of quadratic gravity to be 0 le gamma , lesssim 5.9times 10^{76}, and -frac{gamma }{4} le beta , lesssim 9.8times 10^{75} - frac{gamma }{4}.
Highlights
S= d4 x √ −g R 2κ + β R2 + γ Rμν Rμν (1) where κ = 8π G 1/M 2 P [MP
We have studied gravitational wave signals from the inspiral phase of a compact binary system within the framework of quadratic gravity
Quadratic gravity has been considered as a truncated approximation of a theory represented by an action written in terms of the powers of curvature tensors
Summary
GeV is the reduced Planck mass in natural units], and β, and γ are the dimensionless parameters. Due to the nonrenormalisability of gravity, these parameters cannot be computed theoretically and must be inferred from experiments. In [26] post-merger formation of the horizonless 2-2 hole has been considered with the characteristic prediction of gravitational echoes during the ringdown phase None of these scenarios are feasible within the consistent effective field theory treatment of quadratic gravity adopted in the current work. 2 we rewrite the action (1) in an equivalent and more convenient form separating out the massive spin-0, and the massive spin-2 fields, and will present their solutions in the linearised approximation Given these solutions we compute the leading order corrections to the waveforms generated by a binary inspiral in Sect. Ters in the scenario, one would not expect that a modification of gravity could be “absorbed”, for example, into a re-scaling of the black hole masses, or any other parameter This provides us with an order-of-magnitude estimate of any possible modification of GR, which is convenient for our analysis, which is already to lowest-order, and can only aspire to find an order-of-magnitude constraint. Conservative constraints on the possible deviation of this waveform from GR already exist, and these constraints can be used to directly constrain our modification of gravity
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