The basic idea of the correspondence is that the classical dynamics of the AdS_{5} gravitational field
correspond to the quantum dynamics of a 4D conformal field theory on the brane. This correspondence
holds at linear perturbative order [129], so that the RS 1-brane infinite AdS_{5} brane-world (without matter
fields on the brane) is equivalently described by 4D general relativity coupled to conformal fields,

- Quantum backreaction due to Hawking radiation in the 4D picture is described as classical dynamics in the 5D picture.
- The black hole evaporates as a classical process in the 5D picture, and there is thus no stationary black hole solution in RS 1-brane.

A further remarkable consequence of this conjecture is that Hawking evaporation is dramatically enhanced, due to the very large number of CFT modes of order . The energy loss rate due to evaporation is

where is the number of light degrees of freedom. Using , this gives an evaporation timescale [406] A more detailed analysis [140] shows that this expression should be multiplied by a factor . Then the existence of stellar-mass black holes on long time scales places limits on the AdSOne can also relate the Oppenheimer–Snyder result to these considerations. In the AdS/CFT picture, the non-vanishing of the Ricci scalar, Equation (176), arises from the trace of the Hawking CFT energy-momentum tensor, as in Equation (178). If we evaluate the Ricci scalar at the black hole horizon, , using , we find

The CFT trace on the other hand is given by , so that Thus the Oppenheimer–Snyder result is qualitatively consistent with the AdS/CFT picture.Clearly the black hole solution, and the collapse process that leads to it, have a far richer structure in the brane-world than in general relativity, and deserve further attention. In particular, two further topics are of interest:

- Primordial black holes in 1-brane RS-type cosmology have been investigated in [210, 185, 184, 313, 91, 384]. High-energy effects in the early universe (see the next Section 5) can significantly modify the evaporation and accretion processes, leading to a prolonged survival of these black holes. Such black holes evade the enhanced Hawking evaporation described above when they are formed, because they are much smaller than .
- Black holes will also be produced in particle collisions at energies , possibly well below the Planck scale. In ADD brane-worlds, where is not ruled out by current observations if , this raises the exciting prospect of observing black hole production signatures in the next-generation colliders and cosmic ray detectors (see [75, 169, 138]).

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