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There have been a number of suggestions that the r = 0 singularity of aspherically symmetric (uncharged) evaporating black hole can be circumvented bya quantum transition to a white hole, which eventually releases all trappedquantum information, consistent with overall unitary evolution of the quantumfields. Some of these scenarios rely on loop quantum gravity to impose aminimum area of two-spheres, but are quite vague on how to deal with black holeevaporation, particularly its endpoint. In this paper I present a rathercomplete toy model for the evolution of the geometry and the effectivestress-energy tensor derived from the geometry via the classical Einsteinequations. Modifications of the Schwarzschild geometry once the formation ofthe black hole is complete are very small outside regions of high curvature,and the curvature never becomes super-Planckian. The evolution of the whitehole is roughlythe time reverse of the formation and evaporation of the blackhole. The mass of the white hole increases as it gradually emits the negativeenergy that flowed into the black hole during its evaporation until the matterand radiaton that collapsed to form the black hole emerges and the white holedisappears. I consider the compatibility of the model with some of the quantumenergy condition proposed in the literature, and the implications for theinterpretation of black hole entropy.

Models for the nonsingular transition of an evaporating black hole into a white hole