We investigate the spectral behavior of scalar fluctuations generated by gravity during inflation and the subsequent reheating phase. We consider a nonperturbative Bogoliubov treatment within the context of pure gravitational reheating. We compute both long- and short-wavelength spectra, first for a massless scalar field, revealing that the spectral index in part of the infrared (IR) regime varies between $-6$ and $-3$, depending on the postinflationary equation of state (EoS), $0\le w_{\varphi }\le 1$. Furthermore, we study the mass-breaking effect of the IR spectrum by including the finite mass, $m_{\chi }$, of the daughter scalar field. We show that for $m_{\chi }/H_{\mathrm{e}}\gtrsim 3/2$, where $H_{\mathrm{e}}$ is the Hubble parameter during inflation, the IR spectrum of scalar fluctuations experiences exponential mass suppression, while for smaller masses, $m_{\chi }/H_{\mathrm{e}}<3/2$, the spectrum remains flat in the IR regime regardless of the postinflationary EoS. For any general EoS, we also compute a specific IR scale, $k_m$, of fluctuations below which the IR spectrum will suffer from this finite mass effect. In the UV regime, oscillations of the inflaton background lead to interference terms that explain the high-frequency oscillations in the spectrum. Interestingly, we find that for any EoS, $1/9\lesssim w_{\varphi }\lesssim 1$, the spectral behavior turns out to be independent of the EoS, with a spectral index $-6$. We have compared this Bogoliubov treatment for the UV regime to perturbative computations with solutions to the Boltzmann equation and found an agreement between the two approaches for any EoS, $0\lesssim w_{\varphi }\lesssim 1$. We also explore the relationship between the gravitational reheating temperature and the reheating EoS employing the nonperturbative analytic approach, finding that reheating can occur for $w_{\varphi }\gtrsim 0.6$.

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• Cosmology
• Evolution of the Universe
• Inflation