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The Third Order Scalar Induced Gravitational Waves

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arxiv 2106.01641 v3 pith:JY6ROEIO submitted 2021-06-03 astro-ph.CO gr-qc

classification astro-ph.COgr-qc
keywords ordergravitationalwavesscalarperturbationsthirdinducedsecond
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Since the gravitational waves were detected by LIGO and Virgo, it has been promising that lots of information about the primordial Universe could be learned by further observations on stochastic gravitational waves background. The studies on gravitational waves induced by primordial curvature perturbations are of great interest. The aim of this paper is to investigate the third order induced gravitational waves. Based on the theory of cosmological perturbations, the first order scalar induces the second order scalar, vector and tensor perturbations. At the next iteration, the first order scalar, the second order scalar, vector and tensor perturbations all induce the third order tensor perturbations. We present the energy density spectrum of the third order gravitational waves for a monochromatic primordial power spectrum. The shape of the energy density spectrum of the third order gravitational waves is different from that of the second order scalar induced gravitational waves. And it is found that the third order gravitational waves sourced by the second order scalar perturbations dominate the energy density spectrum.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Suppression of the induced gravitational wave background due to third-order perturbations

    astro-ph.CO 2025-09 conditional novelty 7.0 of 10

    Third-order scalar-tensor correlations suppress the induced gravitational wave background, and some of these new contributions diverge in the ultraviolet.

  2. Cosmological constraints on small-scale primordial non-Gaussianity

    astro-ph.CO 2025-05 conditional novelty 4.0 of 10

    Current pulsar-timing, CMB, BAO and PBH data constrain the small-scale local f_NL to -10.0 < f_NL < 1.2 for a monochromatic primordial power spectrum, with that constraint conditional on the spectral amplitude A_zeta = 10^-2.

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