Order-Unity Correction to Hawking Radiation

When a black hole first forms, the properties of the emitted radiation as measured by observers near future null infinity are very close to the 1974 prediction of Hawking. However, deviations grow with time and become of order unity after a time t similar to M-i(7/3), where M-i is the initial mass in Planck units. After an evaporation time, the corrections are large: the angular distribution of the emitted radiation is no longer dominated by low multipoles, with an exponential falloff at high multipoles. Instead, the radiation is redistributed as a power-law spectrum over a broad range of angular scales, all the way down to the scale Delta theta similar to 1/M-i, beyond which there is exponential falloff. This effect is a quantum gravitational effect, whose origin is the spreading of the wave function of the black hole's center-of-mass location caused by the kicks of the individual outgoing quanta, discovered by Page in 1980. The modified angular distribution of the Hawking radiation has an important consequence: the number of soft hair modes that can effectively interact with outgoing Hawking quanta increases from the handful of modes at low multipoles l to a large number of modes, of order similar to M-i(2). We argue that this change unlocks the Hawking-Perry-Strominger mechanism for purifying the Hawking radiation.

Automated summary

When a black hole first forms, the emitted radiation properties match Hawking's prediction, but deviations grow over time. After a period, the angular distribution of radiation is reshuffled due to quantum gravitational effects, potentially unlocking a mechanism to purify Hawking radiation.