Hawking radiation inside a charged black hole

Here we analyze the Hawking radiation detected by an inertial observer in an arbitrary position in a Reissner-Nordstrom spacetime, with special emphasis on the asymptotic behavior of the Hawking spectrum as an observer approaches the inner or outer horizon. Two different methods are used to analyze the Hawking flux: first, we calculate an effective temperature quantifying the rate of exponential redshift experienced by an observer from an emitter's vacuum modes, which reproduces the Hawking effect provided the redshift is sufficiently adiabatic. Second, we compute the full Bogoliubov graybody spectrum observed in the three regimes where the wave equation can be solved analytically (at infinity and at the outer and inner horizons). We find that for an observer at the event horizon, the effective Hawking temperature is finite and becomes negative when (Q/M)2 > 8/9, while at the inner horizon, the effective temperature is always negative and infinite in every direction the observer looks, coinciding with an ultraviolet-divergent spectrum.

Automated summary

In this paper, the Hawking radiation detected by an inertial observer in a Reissner-Nordstrom spacetime is analyzed, with a focus on the asymptotic behavior of the Hawking spectrum as the observer approaches the inner or outer horizon. Two different methods are used to analyze the Hawking flux: an effective temperature is calculated to quantify the redshift experienced by the observer, and the full Bogoliubov graybody spectrum is computed in analytically solvable regions. The results show that the effective Hawking temperature is finite and becomes negative at the event horizon for certain conditions, while it is always negative and infinite at the inner horizon.