Properties of Black Hole Radiation From Tunnelling

Abstract

We consider the space-time associated with the evaporation of a black hole by quantum mechanical tunnelling events. It is shown that the surface through which tunnelling occurs is distinct from the global event horizon, and that this has consequences for the radiation reaching future null infinity. A spherical collapse process is modelled, and the radiation expected to be observed at future null infinity is calculated. It is shown that external observers witness an evaporation process that begins as the tunnelling surface is exposed, and ends as the collapsing object passes behind its event horizon. The sensitivity of emitted radiation to the collapse process is illustrated.