1993/02/10 by Malcolm J. Perry, Edward Teo
Mathematics · Physics and Astronomy · #Black Holes and Theoretical Physics #Black hole (networking) #Classical mechanics #Cosmology and Gravitation Theories #General relativity #Geometry #Gravitational singularity #Limit (mathematics) #Mathematical analysis #Mathematical physics #Mathematics #Naked singularity #Noncommutative and Quantum Gravity Theories #Physics #Quantum #Quantum mechanics #Schwarzschild metric #Schwarzschild radius #Semiclassical physics #Sequence (biology) #Singularity #Space (punctuation) #Space time #Spacetime #String (physics) #String theory #Symmetry (geometry) #Theoretical physics #Wormhole #hep-th
paper · pdf · doi:10.1103/physrevlett.70.2669
published as Phys.Rev.Lett. 70 (1993) 2669-2672 · 9 pages, latex, DAMTP R93/1
arxiv created 1993/02/10 · openalex publication_date 1993/05/03 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
In the semiclassical limit, the two-dimensional space-time which emerges from string theory is a black hole similar to the Schwarzschild solution. However, we find that in the exact space-time, the singularity is replaced by a regular surface of time-reflection symmetry. The maximally extended space-time thus consists of an infinite sequence of asymptotically flat regions linked by wormholes, rather analogous to the Reissner-Nordstr"om space-time except that there are no singularities in this case. We also calculate the mass and temperature associated with this space-time.