Primordial black hole induced gravitational waves in f(R) gravity

Ultra-light primordial black holes (PBHs) with masses $M_\mathrm{PBH}<5\times 10^{8}\mathrm{g}$ can trigger an early matter-dominated (eMD) era before Big Bang Nucleosynthesis (BBN) and reheat the Universe through their evaporation. Notably, the initial isocurvature in nature PBH energy density fluctuations can induce abundantly gravitational waves (GWs) due to second-order gravitational effects. In this work, we study this induced GW signal within the context of $f(R)$ gravity theories investigating the effect of $f(R)$ gravity on the behaviour of scalar perturbations during the PBH-driven eMD era as well as on the source of the second-order induced tensor modes. In particular, we focus on two very minimal $f(R)$ models, that is $R^2$ and $R^{1+\epsilon}$, with $\epsilon\ll 1$, gravity theories as illustrative examples, finding at the end that $R^2$ gravity presents very small deviations from general relativity (GR) at the level of both the scalar and tensor perturbations. However, $R^{1+\epsilon}$ gravity features a different behaviour, exhibiting in particular an exponential growth of scalar perturbations during a matter-dominated era. This unique feature leads ultimately to an enhanced induced GW signal even for very small initial PBH abundances, being characterized by a linear frequency scaling on large infrared scales away from the peak frequency, i.e. $\Omega_\mathrm{GW}(k)\propto f$ for $f\ll f_\mathrm{peak}$, and a spiky behaviour close to the non-linear cut-off scale below which perturbation theory breaks down. Interestingly, one finds as well that the induced GW signal can be well within the sensitivity curves of GW detectors, namely that of LISA, ET, BBO and SKA.