The gravitational<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>S</mml:mi></mml:math>matrix

Giddings, Steven B.; Porto, Rafael A.

doi:10.1103/physrevd.81.025002

Cited by 75 publications

(81 citation statements)

References 75 publications

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“…In fact, as shown in [23], before the BH formation an eikonal barrier may well form. In this case eikonal amplitudes (exchange of many soft gravitons) become important preventing hard energy transfers through a single graviton line which would encode information about short distance physics.…”

Section: Trans-planckian Gravity Is Ir Gravitymentioning

confidence: 99%

Physics of trans-Planckian gravity

2011

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We study the field theoretical description of a generic theory of gravity flowing to Einstein General Relativity in IR. We prove that, if ghost-free, in the weakly coupled regime such a theory can never become weaker than General Relativity. Using this fact, as a byproduct, we suggest that in a ghost-free theory of gravity trans-Planckian propagating quantum degrees of freedom cannot exist. The only physical meaning of a trans-Planckian pole is the one of a classical state (Black Hole) which is described by the light IR quantum degrees of freedom and gives exponentially-suppressed contributions to virtual processes. In this picture Einstein gravity is UV self-complete, although not Wilsonian, and sub-Planckian distances are unobservable in any healthy theory of gravity. We then finally show that this UV/IR correspondence puts a severe constraint on any attempt of conventional Wilsonian UV-completion of trans-Planckian gravity. Specifically, there is no well-defined energy domain in which gravity could become asymptotically weak or safe.

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Section: Trans-planckian Gravity Is Ir Gravitymentioning

confidence: 99%

Physics of trans-Planckian gravity

2011

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“…A possible initial non-vanishing electric charge is quickly almost neutralized because of the highly ionized host environment, and the residual equilibrium charge is very small and completely negligible for the spacetime geometry (Bambi et al 2009a;Bambi 2017a). On the contrary, macroscopic deviations from the Kerr metric are possible in the presence of exotic matter (Herdeiro, & Radu 2014;Herdeiro et al 2016), quantum gravity effects (Dvali, & Gomez 2013;Giddings 2017;Giddings, & Psaltis 2018), as well as in a number of modified theories of gravity (Kleihaus et al 2011;Sotiriou, & Zhou 2014;Ayzenberg, & Yunes 2014).…”

Section: Introductionmentioning

confidence: 99%

Tests of the Kerr Hypothesis with GRS 1915+105 Using Different relxill Flavors

Zhang

Abdikamalov

Ayzenberg

et al. 2019

ApJ

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In a previous paper, we tried to test the Kerr nature of the stellar-mass black hole in GRS 1915+105 by analyzing NuSTAR data of 2012 with our reflection model relxill nk. We found that the choice of the intensity profile of the reflection component is crucial and eventually we were not able to get any constraint on the spacetime metric around the black hole in GRS 1915+105. In the present paper, we study the same source with Suzaku data of 2007. We confirm that the intensity profile plays an important role, but now we find quite stringent constraints consistent with the Kerr hypothesis. The key differences with respect to our previous study are likely the lower disk temperature in the Suzaku observation and the higher energy resolution near the iron line of the Suzaku data. We also apply different relxill flavors (different descriptions of the coronal spectrum and variable disk electron density) obtaining essentially the same results. We thus conclude that this choice is not very important for our tests of the Kerr hypothesis while the intensity profile does play an important role, and that with high quality data it is possible to measure both the spacetime metric and the intensity profile.

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“…Previous attempts to understand and resolve the information paradox include the S-matrix approach [7,[10][11][12][13] and the fuzzball approach [14][15][16]. Both share some ingredients and conclusions with the proposed resolution of the information paradox.…”

Section: Introductionmentioning

confidence: 99%

Origin of the blackhole information paradox

Brustein

2014

Fortschritte der Physik

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It is argued that the blackhole information paradox originates from treating the blackhole geometry as strictly classical. It is further argued that the theory of quantum fields in a classical curved space with a horizon is an ill posed problem. If the geometry is allowed to fluctuate quantum mechanically, then the horizon effectively disappears.The sharp horizon emerges only in the classical limit when the ratio of the Compton wavelength of the black hole to its Schwarzschild radius vanishes. The region of strong gravity that develops when matter collapses to form the blackhole remains visible to the whole of spacetime and has to be described by a microscopic theory of strong gravity.The arguments imply that the information paradox is demoted from a paradox involving fundamental principles of physics to the problem of describing how matter at the highest densities gravitates.

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The gravitationalSmatrix

Cited by 75 publications

References 75 publications

Physics of trans-Planckian gravity

Physics of trans-Planckian gravity

Tests of the Kerr Hypothesis with GRS 1915+105 Using Different relxill Flavors

Origin of the blackhole information paradox

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