1995/05/10 by Jacob D. Bekenstein, V. F. Mukhanov, V.F. Mukhanov · 15 citations
Physics and Astronomy · #Black Holes and Theoretical Physics #Noncommutative and Quantum Gravity Theories #Quantum Electrodynamics and Casimir Effect #gr-qc #hep-th #quant-ph
paper · pdf · doi:10.1016/0370-2693(95)01148-j
published as Phys.Lett. B360 (1995) 7-12 · RevTeX, 9 pages
arxiv created 1995/05/10 · openalex publication_date 1995/10/01 · arxiv updated 2009/11/30 · openalex created_date 2017/03/16 · openalex updated_date 2026/07/28
We develop the idea that, in quantum gravity where the horizon fluctuates, a black hole should have a discrete mass spectrum with concomitant line emission. Simple arguments fix the spacing of the lines, which should be broad but unblended. Assuming uniformity of the matrix elements for quantum transitions between near levels, we work out the probabilities for the emission of a specified series of quanta and the intensities of the spectral lines. The thermal character of the radiation is entirely due to the degeneracy of the levels, the same degeneracy that becomes manifest as black hole entropy. One prediction is that there should be no lines with wavelength of order the black hole size or larger. This makes it possible to test quantum gravity with black holes well above Planck scale.