Abstract:Quantum gravity is expected to resolve the singularities of classical general relativity. Based on destructive interference of singular spacetime-configurations in the path integral, we find that higher-order curvature terms may allow to resolve black-hole singularities both in the spherically symmetric and axisymmetric case. In contrast, the Einstein action does not provide a dynamical mechanism for singularity-resolution through destructive interference of these configurations.
“…The last principle distinguishes our construction from other work in spinning spacetimes, e.g., [18,22,23,25,26,28,29,32,[34][35][36]. As we will see, its implementation results in distinct new spacetime and image features.…”
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confidence: 95%
“…In the first strategy, black-hole solutions are derived in gravity theories beyond GR [18,[20][21][22][23][24][25][26][27][28][29][30][31][32][33][34][35][36]. This strategy has a e-mail: eichhorn@cp3.sdu.dk b e-mail: a.held@imperial.ac.uk (corresponding author) two main disadvantages: First, it is impossible to cover every conceivable theory beyond GR.…”
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confidence: 99%
“…It follows from a (classical or quantum) effective field theory point of view on new physics which implies that deviations from GR set in beyond a critical value of the local curvature. It is motivated by several research lines, where quantum or classical modifications of GR follow effective field theory principles, both for black holes, e.g., [45][46][47][48][49][50][51][52] and beyond, e.g., [53][54][55][56][57][58][59][60][61]. Within the highly restricted setting of spherical symmetry, principles (i)-(iv) have been successfully implemented, cf.…”
To understand the true nature of black holes, fundamental theoretical developments should be linked all the way to observational features of black holes in their natural astrophysical environments. Here, we take several steps to establish such a link. We construct a family of spinning, regular black-hole spacetimes based on a locality principle for new physics and analyze their shadow images. We identify characteristic image features associated to regularity (increased compactness and relative stretching) and to the locality principle (cusps and asymmetry) that persist in the presence of a simple analytical disk model. We conjecture that these occur as universal features of distinct classes of regular black holes based on different sets of construction principles for the corresponding spacetimes.
“…The last principle distinguishes our construction from other work in spinning spacetimes, e.g., [18,22,23,25,26,28,29,32,[34][35][36]. As we will see, its implementation results in distinct new spacetime and image features.…”
mentioning
confidence: 95%
“…In the first strategy, black-hole solutions are derived in gravity theories beyond GR [18,[20][21][22][23][24][25][26][27][28][29][30][31][32][33][34][35][36]. This strategy has a e-mail: eichhorn@cp3.sdu.dk b e-mail: a.held@imperial.ac.uk (corresponding author) two main disadvantages: First, it is impossible to cover every conceivable theory beyond GR.…”
mentioning
confidence: 99%
“…It follows from a (classical or quantum) effective field theory point of view on new physics which implies that deviations from GR set in beyond a critical value of the local curvature. It is motivated by several research lines, where quantum or classical modifications of GR follow effective field theory principles, both for black holes, e.g., [45][46][47][48][49][50][51][52] and beyond, e.g., [53][54][55][56][57][58][59][60][61]. Within the highly restricted setting of spherical symmetry, principles (i)-(iv) have been successfully implemented, cf.…”
To understand the true nature of black holes, fundamental theoretical developments should be linked all the way to observational features of black holes in their natural astrophysical environments. Here, we take several steps to establish such a link. We construct a family of spinning, regular black-hole spacetimes based on a locality principle for new physics and analyze their shadow images. We identify characteristic image features associated to regularity (increased compactness and relative stretching) and to the locality principle (cusps and asymmetry) that persist in the presence of a simple analytical disk model. We conjecture that these occur as universal features of distinct classes of regular black holes based on different sets of construction principles for the corresponding spacetimes.
“…On the other hand in the Lorentztian signature the more varying actions contribute less. Hence for the actions neighbouring the infinite one the variation is significant and the neighbouring ones do cancel each other, see 1 . This notion has recently received significant attention in the literature, see [2][3][4] for the cosmological considerations and 1,4 for the black hole ones.…”
Section: Introductionmentioning
confidence: 99%
“…Hence for the actions neighbouring the infinite one the variation is significant and the neighbouring ones do cancel each other, see 1 . This notion has recently received significant attention in the literature, see [2][3][4] for the cosmological considerations and 1,4 for the black hole ones. Since it is expected that the quantum gravity should resolve the black-hole singularity problem, one may ask which of the microscopic actions remain finite for non-singular black holes and conversely interfere destructively for the singular ones.…”
In this work, we elaborate on the finite action for wormholes in higher derivative theories. Both non-traversable and traversable wormholes in theories with higher curvature invariants posses finite action.
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