Study of eccentric binaries in Horndeski gravity

Chowdhuri, Abhishek; Bhattacharyya, Arpan

doi:10.1103/physrevd.106.064046

Cited by 17 publications

(6 citation statements)

References 92 publications

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“…Therefore, the choice of typical alternative gravitational theory [25][26][27][28][29][30][31][32] and the calculation of GW waveforms in the theory have crucial roles. For example, the gravitational waveforms have been derived in Brans-Dicke (BD) gravity [33][34][35], Einstein-aether theory [35][36][37], screen modified gravity [38][39][40][41], and Horndeski theory [42]. Current and future GW observations can constrain these gravitational theories with high accuracy [43][44][45][46][47][48][49][50][51][52].…”

Section: Jcap04(2023)006 1 Introductionmentioning

confidence: 99%

Gravitational waveform and polarization from binary black hole inspiral in dynamical Chern-Simons gravity: from generation to propagation

Zhao

Qiao

Liu

et al. 2023

J. Cosmol. Astropart. Phys.

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We calculate the gravitational waveform radiated from spinning black holes (BHs) binary in dynamical Chern-Simons (dCS) gravity. The equation of motion (EOM) of the spinning binary BHs is derived based on the modified Mathisson-Papapetrou-Dixon equation for the spin-aligned circular orbits. The leading-order effects induced by the dCS theory contain spin-spin interaction and monopole-quadrupole interaction, which influences both the EOM of the binary system and corresponding gravitational waveform at the second post-Newtonian (PN) order (i.e., 2PN order). After reporting the waveforms, we investigate the polarization modes of gravitational waves (GWs) in dCS theory. None of the extra modes appears in this theory up to the considered PN order. Moreover, since the time scale of the binary merger is much smaller than that of the cosmological expansion, the parity-violating effect of the dCS theory does not appear in the process of GW generation. However, during the process of GW propagation, amplitude birefringence, a typical parity-violating effect, makes plus and cross modes convert to each other, which modifies the gravitational waveform at 1.5PN order.

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Section: Jcap04(2023)006 1 Introductionmentioning

confidence: 99%

Gravitational waveform and polarization from binary black hole inspiral in dynamical Chern-Simons gravity: from generation to propagation

Zhao

Qiao

Liu

et al. 2023

J. Cosmol. Astropart. Phys.

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show abstract

“…However, the scalar field is massless in their study. Recently, radiation from eccentric binaries in the classical framework has been studied in Horndeski theories with the massless scalar field and without the screening assumption [66].…”

Section: Jcap03(2023)008mentioning

confidence: 99%

Gravitational radiation from binary systems in f(R) gravity: A semi-classical approach

Narang

Mohanty

Jana³

2023

J. Cosmol. Astropart. Phys.

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The rate of energy loss and orbital period decay of quasi- stable compact binary systems are derived in f(R) theory of gravity using the method of a single vertex graviton emission process from a classical source. After linearising the f(R) action written in an equivalent scalar-tensor format in the Einstein frame, we identify the appropriate interaction terms between the massless spin-2 tensor mode, massive scalar mode, and the energy momentum tensor. The definition of the scalar field is related to the f(R) models. Then using the interaction vertex we compute the rate of energy loss due to spin-2 quadrupole radiation, which comes out to be the same as the Peter-Mathews formula with a multiplication factor, and also the energy loss due to the scalar dipole radiation. The total energy loss is the sum of these two contributions. Our derivation is most general as it is applicable for both arbitrary eccentricity of the binary orbits and arbitrary mass of the scalar field. Using the derived theoretical formula for the period decay of the binary systems, we compare the predictions of f(R) gravity and general relativity for the observations of four binary systems, i.e. Hulse-Taylor Binary, PSR J1141-6545, PSR J1738+0333, and PSR J0348+0432. Thus we put bound on three well-known f(R) dark energy models, namely the Hu-Sawicki, the Starobinsky, and the Tsujikawa model. We get the best constraint on f'(R 0)-1 (where R 0 is the scalar curvature of the Universe at the present epoch) from the Tsujikawa model, i.e |f'(R 0)-1| < 2.09 × 10-4. This bound is stronger than those from most of the astrophysical observations and even some cosmological observations.

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“…In Refs. [98,102], the effective GW stress-energy tensor t µν in Horndeski theories was derived under a shortwavelength approximation. This is based on the approximation that the wavelength of GWs is much smaller than a typical background curvature scale [103].…”

Section: A Time Variation Of Orbital Frequencymentioning

confidence: 99%

Inspiral gravitational waveforms from compact binary systems in Horndeski gravity

Higashino¹,

Tsujikawa²

2022

Preprint

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In a subclass of Horndeski theories with the speed of gravity equivalent to that of light, we study gravitational radiation emitted during the inspiral phase of compact binary systems. We compute the waveform of scalar perturbations under a post-Newtonian expansion of energy-momentum tensors of point-like particles that depend on a scalar field. This scalar mode not only gives rise to breathing and longitudinal polarizations of gravitational waves, but it is also responsible for scalar gravitational radiation in addition to energy loss associated with transverse and traceless tensor polarizations. We calculate the Fourier-transformed gravitational waveform of two tensor polarizations under a stationary phase approximation and show that the resulting waveform reduces to the one in a parametrized post-Einsteinian (ppE) formalism. The ppE parameters are directly related to a scalar charge in the Einstein frame, whose existence is crucial to allow the deviation from General Relativity (GR). We apply our general framework to several concrete theories and show that a new theory of spontaneous scalarization with a higher-order scalar kinetic term leaves interesting deviations from GR that can be probed by the observations of gravitational waves emitted from neutron star-black hole binaries. If the scalar mass exceeds the order of typical orbital frequencies ω 10 −13 eV, which is the case for a recently proposed scalarized neutron star with a self-interacting potential, the gravitational waveform practically reduces to that in GR.

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Study of eccentric binaries in Horndeski gravity

Cited by 17 publications

References 92 publications

Gravitational waveform and polarization from binary black hole inspiral in dynamical Chern-Simons gravity: from generation to propagation

Gravitational waveform and polarization from binary black hole inspiral in dynamical Chern-Simons gravity: from generation to propagation

Gravitational radiation from binary systems in f(R) gravity: A semi-classical approach

Inspiral gravitational waveforms from compact binary systems in Horndeski gravity

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