2015/06/30 by Alejandro Corichi, Parampreet Singh · 153 citations
Physics and Astronomy · #Black Holes and Theoretical Physics #Black hole (networking) #Initial singularity #Loop quantum gravity #Noncommutative and Quantum Gravity Theories #Quantization (signal processing) #Quantum gravity #Relativity and Gravitational Theory #Schwarzschild metric #Schwarzschild radius #Semiclassical physics #Singularity #Spacetime #astro-ph.CO #gr-qc #hep-th
paper · pdf · doi:10.1088/0264-9381/33/5/055006
published in Classical and Quantum Gravity 33(5), 055006 (IOP Publishing) · Revised version. Comparison with Ashtekar-Bojowald quantization expanded. A figure showing dependence of the white hole mass on the fiducial cell in Ashtekar-Bojowald quantization added. To appear in CQG
arxiv created 2015/12/22 · openalex publication_date 2016/02/12 · arxiv updated 2016/02/15 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
The loop quantization of the Schwarzschild interior region, as described by a homogeneous anisotropic Kantowski–Sachs model, is re-examined. As several studies of different—inequivalent—loop quantizations have shown, to date there exists no fully satisfactory quantum theory for this model. This fact poses challenges to the validity of some scenarios to address the black hole information problem. Here we put forward a novel viewpoint to construct the quantum theory that builds from some of the models available in the literature. The final picture is a quantum theory that is both independent of any auxiliary structure and possesses a correct low curvature limit. It represents a subtle but non-trivial modification of the original prescription given by Ashtekar and Bojowald. It is shown that the quantum gravitational constraint is well defined past the singularity and that its effective dynamics possesses a bounce into an expanding regime. The classical singularity is avoided, and a semiclassical spacetime satisfying vacuum Einstein's equations is recovered on the 'other side' of the bounce. We argue that such a metric represents the interior region of a white-hole spacetime, but for which the corresponding 'white hole mass' differs from the original black hole mass. Furthermore, we find that the value of the white hole mass is proportional to the third power of the starting black hole mass.