Unitary paradox of cosmological perturbations

Abstract

If we interpret the Bekenstein-Hawking entropy of the Hubble horizon as thermodynamic entropy, then the entanglement entropy of the superhorizon modes of curvature perturbation entangled with the subhorizon modes will exceed the Bekenstein-Hawking bound at some point; we call this the unitary paradox of cosmological perturbations by analogy with black hole. In order to avoid a fine-tuned problem, the paradox must occur during the inflationary era at the critical time $t_c=\ln (3\sqrt{\pi }/\sqrt{2}{\epsilon }_H{H}_{inf})/2H_{inf}$ (in Planck units), where ${\epsilon }_H=-\dot{H}/H^2$ is the first Hubble slow-roll parameter and $H_{inf}$ is the Hubble rate during inflation. If we instead accept the fine-tuned problem, then the paradox will occur during the dark energy era at the critical time $t_c^{\prime }=\ln (3\sqrt{\pi }{H}_{inf}/\sqrt{2}f{e}^{2N}{H}_{\Lambda }^2)/2H_{\Lambda }$, where $H_{\Lambda }$ is the Hubble rate dominated by dark energy, $N$ is the total number of e-folds of inflation, and $f$ is a purification factor that takes the range $0<f<3\sqrt{\pi }{H}_{inf}/\sqrt{2}{e}^{2N}{H}_{\Lambda }^2$.

13 pages, 3 figures; close to published version

References in corpus (1)

• The central dogma and cosmological horizons

Cited by in corpus (1)

• Time-System Entanglement and Special Relativity