Quantum fluctuating CGHS geometries and the information paradox

Abstract

We study Hawking radiation on the quantum spacetime generated by a quantum ingoing null shell in the 2d theory proposed by Callan-Giddings-Harvey-Strominger (CGHS). The quantum spacetime is a superposition of classical geometries with uncertainty in position and momentum of the collapsing shell. The Hawking radiation spectrum is computed, revealing a non-thermal behaviour for finite time as well as a dependence on the shell's physical degrees of freedom. Hawking radiation's dependence on the collapsing shell becomes irrelevant in the late time approximation as we reach i + since the radiation's temperature depends exclusively on the cosmological constant. However, we argue that the information of the quantum state of a collapsing shell can be read from the Hawking radiation if we perform measurements at I + R taking into account backreaction effects. *

On the $$\beta $$-decay of the accelerated proton and neutrino oscillations: a three-flavor description with CP violation

“…In this regard, we envisage that some new features might come into play, as for example the necessity of a full-fledged QFT treatment of neutrino mixing instead of the Pontecorvo quantum mechanical one [24], or the possibility to violate the thermality of the Unruh effect when considering mixed fields [36]. Note that similar non-thermal distortions of the Unruh-Hawking spectrum have been recently highlighted also in other contexts, such as the emission on the background of a quantum collapsing null shell [37], the polymer (loop) quantization for the calculation of the two-point function along Rindler trajectories [38], the Casimir effect between uniformly accelerated atoms [39] and the Generalized Uncertainty Principle framework [40].…”

Quantum fluctuating geometries and the information paradox II

“…Figure (5) depicts this departure which is most apparent in (5a). The oscillatory behavior at the end of the plot is not to be trusted.…”

“…To do the explicit calculation we need an expression for (18) that we can handle when ω 1 ∼ ω 2 . Approximating the integrand to the lowest order in ∆ω/ω both in amplitude and in phase in all the factors involved, we get [5],…”