Scalar stochastic gravitational-wave background in Brans-Dicke theory of gravity

Abstract

We study the scalar stochastic gravitational-wave background (SGWB) from astrophysical sources, including compact binary mergers and stellar collapses, in the Brans-Dicke theory of gravity. By contrast to tensor waves, the scalar SGWB predominantly arises from stellar collapses. These collapses not only take place at higher astrophysical rates but also emit more energy. This is because, unlike tensor radiation which mainly starts from quadrupole order, the scalar perturbation can be excited by changes in the monopole moment. In particular, in the case of stellar collapse into a neutron star or a black hole, the monopole radiation, at frequencies below 100 Hz, is dominated by the memory effect. At low frequencies, the scalar SGWB spectrum follows a power law of Ω_S ∝ f^α, with α = 1. We predict that Ω_S is inversely proportional to the square of ω_(BD) + 2, with (ω_(BD) + 2)^2Ω_S (f = 25 Hz) = 2.8 × 10^(−6). We also estimate the detectability of the scalar SGWB for current and third-generation detector networks and the bound on ω_(BD) that can be imposed from these observations.

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