PIRSA:14030115

Possible Astrophysical Observables of Quantum Gravity Effects near Black Holes

Pen, U. (2014). Possible Astrophysical Observables of Quantum Gravity Effects near Black Holes. Perimeter Institute. https://pirsa.org/14030115

Pen, Ue-Li. Possible Astrophysical Observables of Quantum Gravity Effects near Black Holes. Perimeter Institute, Mar. 27, 2014, https://pirsa.org/14030115 

          @misc{ pirsa_PIRSA:14030115,
            doi = {10.48660/14030115},
            url = {https://pirsa.org/14030115},
            author = {Pen, Ue-Li},
            keywords = {Quantum Gravity},
            language = {en},
            title = {Possible Astrophysical Observables of Quantum Gravity Effects near Black Holes},
            publisher = {Perimeter Institute},
            year = {2014},
            month = {mar},
            note = {PIRSA:14030115 see, \url{https://pirsa.org}}
          }

Ue-Li Pen

Canadian Institute for Theoretical Astrophysics (CITA)

Talk number
PIRSA:14030115
Collection
Talk Type
Subject
Abstract
Recent implications of results from quantum information theory applied to black holes has led to the confusing conclusions that requires either abandoning the equivalence principle (e.g. the firewall picture), or the no-hair theorem (e.g. the fuzzball picture), or even more unpalatable options. The recent discovery of a pulsar orbiting a black hole opens up new possibilities for tests of theories of gravity. We examine possible observational effects of semiclassical quantum gravity in the vicinity of black holes, as probed by pulsars and event horizon telescope imaging of flares. Pulsar radiation is observable at wavelengths only two orders of magnitude shorter than the Hawking radiation, so precision interferometry of lensed pulsar images may shed light on the quantum gravitational processes and interaction of Hawking radiation with the spacetime near the black hole. This paper discusses the impact on the pulsar radiation interference pattern, which is observable through the modulation index in the foreseeable future, and discusses a possible classical limit of BHC.