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<title>Edward Witten - INSPIRE</title>
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<title>Instantons and the Large N=4 Algebra</title>
<description><span>We investigate the differential geometry of the moduli space of instantons on ${\mathrm S}^3 \times {\mathrm S}^1$. Extending previous results, we show that a sigma-model with this target space can be expected to possess a large ${\mathcal N}=4$ superconformal symmetry, supporting speculations that this sigma-model may be dual to Type IIB superstring theory on $\mathrm{AdS}_3 \times {\mathrm S}^3 \times {\mathrm S}^3\times {\mathrm S}^1$.&nbsp; &nbsp;The sigma-model is parametrized by three integers -- the
rank of the gauge group, the instanton number, and a ``level'' (the integer coefficient of a topologically nontrivial $B$-field, analogous to a WZW level). These integers are expected to correspond to two five-brane charges and a one-brane charge.&nbsp; &nbsp;The sigma-model is weakly coupled when the level,&nbsp; conjecturally corresponding to one of the five-brane changes, becomes very large, keeping the other parameters fixed.&nbsp; The central charges of the large ${\mathcal N}=4$ algebra agree, at least semiclassically, with expectations from the duality.</span></description>
<link>https://inspirehep.net/literature/2812078</link>
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<pubDate>Wed, 31 Jul 2024 04:28:30 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
</item>
<item>
<title>Scale and Conformal Invariance in 2d Sigma Models, with an Application to N=4 Supersymmetry</title>
<description><span>By adapting previously known arguments concerning Ricci flow and the c-theorem, we give a direct proof that in a two-dimensional sigma-model with compact target space, scale invariance implies conformal invariance in perturbation theory. This argument, which applies to a general sigma-model constructed with a target space metric and B-field, is in accord with a more general proof in the literature that applies to arbitrary two-dimensional quantum field theories. Models with extended supersymmetry and a B-field are known to provide interesting test cases for the relation between scale invariance and conformal invariance in sigma-model perturbation theory. We give examples showing that in such models, the obstructions to conformal invariance suggested by general arguments can actually occur in models with target spaces that are not compact or complete. Thus compactness of the target space, or at least a suitable condition of completeness, is necessary as well as sufficient to ensure that scale invariance implies conformal invariance in models of this type.</span></description>
<link>https://inspirehep.net/literature/2782301</link>
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<pubDate>Wed, 01 May 2024 03:53:57 GMT</pubDate>
<author>Georgios Papadopoulos (King's Coll. London, Dept. Math), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>invariance: conformal</category>
<category>invariance: scale</category>
<category>dimension: 2</category>
<category>supersymmetry</category>
<category>flow: Ricci</category>
<category>sigma model</category>
<category>perturbation theory</category>
<category>mathematical methods</category>
<category>space: compact</category>
</item>
<item>
<title>Liouville Theory: An Introduction to Rigorous Approaches</title>
<description><span>In recent years, a surprisingly direct and simple rigorous understanding of quantum Liouville theory has developed. We aim here to make this material more accessible to physicists working on quantum field theory.</span></description>
<link>https://inspirehep.net/literature/2773427</link>
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<pubDate>Wed, 03 Apr 2024 03:50:18 GMT</pubDate>
<author>Sourav Chatterjee (Stanford U.), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>field theory: Liouville</category>
</item>
<item>
<title>A background-independent algebra in quantum gravity A Background Independent Algebra in Quantum Gravity</title>
<description><span>We propose an algebra of operators along an observer’s worldline as a background-independent algebra in quantum gravity. In that context, it is natural to think of the Hartle-Hawking no boundary state as a universal state of maximum entropy, and to define entropy in terms of the relative entropy with this state. In the case that the only spacetimes considered correspond to de Sitter vacua with different values of the cosmological constant, this definition leads to sensible results.</span><br><span>We propose an algebra of operators along an observer's worldline as a background-independent algebra in quantum gravity. In that context, it is natural to think of the Hartle-Hawking no boundary state as a universal state of maximum entropy, and to define entropy in terms of the relative entropy with this state. In the case that the only spacetimes considered correspond to de Sitter vacua with different values of the cosmological constant, this definition leads to sensible results.</span></description>
<link>https://inspirehep.net/literature/2686072</link>
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<pubDate>Tue, 08 Aug 2023 08:29:45 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>Cosmological models</category>
<category>de Sitter space</category>
<category>operator: algebra</category>
<category>vacuum state: de Sitter</category>
<category>entropy</category>
<category>quantum gravity</category>
<category>cosmological constant</category>
<category>space-time</category>
<category>background</category>
</item>
<item>
<title>$ \mathcal{N} $ = 2 JT supergravity and matrix models $N=2$ JT Supergravity and Matrix Models $\mathcal{N}=2$ JT Supergravity and Matrix Models</title>
<description><span>Generalizing previous results for $ \mathcal{N} $ = 0 and $ \mathcal{N} $ = 1, we analyze $ \mathcal{N} $ = 2 JT supergravity on asymptotically AdS$_{2}$ spaces with arbitrary topology and show that this theory of gravity is dual, in a holographic sense, to a certain random matrix ensemble in which supermultiplets of different R-charge are statistically independent and each is described by its own $ \mathcal{N} $ = 2 random matrix ensemble. We also analyze the case with a time-reversal symmetry, either commuting or anticommuting with the R-charge. In order to compare supergravity to random matrix theory, we develop an $ \mathcal{N} $ = 2 analog of the recursion relations for Weil-Petersson volumes originally discovered by Mirzakhani in the bosonic case.</span><br><span>Generalizing previous results for $N=0$ and $N=1$, we analyze $N=2$ JT supergravity on asymptotically AdS${}_2$ spaces with arbitrary topology and show that this theory of gravity is dual, in a holographic sense, to a certain random matrix ensemble in which supermultiplets of different $R$-charge are statistically independent and each is described by its own $N=2$ random matrix ensemble. We also analyze the case with a time-reversal symmetry, either commuting or anticommuting with the $R$-charge. In order to compare supergravity to random matrix theory, we develop an $N=2$ analog of the recursion relations for Weil-Petersson volumes originally discovered by Mirzakhani in the bosonic case.</span></description>
<link>https://inspirehep.net/literature/2664145</link>
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<pubDate>Thu, 01 Jun 2023 02:55:33 GMT</pubDate>
<author>Gustavo J. Turiaci (Princeton, Inst. Advanced Study, Washington U., Seattle), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>Black Holes</category>
<category>Extended Supersymmetry</category>
<category>Matrix Models</category>
<category>matrix model: random</category>
<category>time reversal: symmetry</category>
<category>supergravity: 2</category>
<category>duality: holography</category>
<category>topology</category>
<category>space: anti-de Sitter</category>
<category>dimension: 2</category>
<category>path integral</category>
<category>black hole</category>
</item>
<item>
<title>Anomalies and Nonsupersymmetric D-Branes</title>
<description><span>We revisit some aspects of D-brane theory from the point of view of anomalies. When the boundary condition on a worldsheet boson is flipped from Neumann to Dirichlet, worldsheet supersymmetry requires also reversing the sign of the boundary condition of the corresponding worldsheet fermion. This induces an anomaly which is a mod 2 anomaly in Type II superstring theory and a mod 8 anomaly in Type I superstring theory. The same anomaly also receives contributions from a sign in the sum over bulk spin structures (in Type IIA superstring theory), Chan-Paton factors of symplectic type (in Type I superstring theory), and Majorana fermions that propagate only on the worldsheet boundary. The need to cancel the anomaly accounts for many properties of supersymmetric and especially nonsupersymmetric D-branes in Type I and Type II superstring theory.</span></description>
<link>https://inspirehep.net/literature/2655986</link>
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<pubDate>Wed, 03 May 2023 03:05:13 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>fermion: Majorana</category>
<category>anomaly</category>
<category>superstring</category>
<category>D-brane</category>
<category>boundary condition</category>
<category>structure</category>
<category>Chan-Paton factor</category>
<category>symplectic</category>
<category>spin</category>
</item>
<item>
<title>The Timelike Tube Theorem in Curved Spacetime The Timelike Tube Theorem in Curved Spacetime</title>
<description><span>The timelike tube theorem asserts that in quantum field theory without gravity, the algebra of observables in an open set ${\mathcal {U}}$ is the same as the corresponding algebra of observables in its “timelike envelope” ${\mathcal {E}}({\mathcal {U}})$, which is an open set that is in general larger. The theorem was originally proved in the 1960’s by Borchers and Araki for quantum fields in Minkowski space. Here we sketch the proof of a version of the theorem for quantum fields in a general real analytic spacetime. Details have appeared elsewhere.</span><br><span>The timelike tube theorem asserts that in quantum field theory without gravity, the algebra of observables in an open set U is the same as the corresponding algebra of observables in its ``timelike envelope'' E(U), which is an open set that is in general larger. The theorem was originally proved in the 1960's by Borchers and Araki for quantum fields in Minkowski space. Here we sketch the proof of a version of the theorem for quantum fields in a general real analytic spacetime. Details have appeared elsewhere.</span></description>
<link>https://inspirehep.net/literature/2646935</link>
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<pubDate>Thu, 30 Mar 2023 03:03:37 GMT</pubDate>
<author>Alexander Strohmaier (Leeds U., Math.), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>space: Minkowski</category>
<category>space-time</category>
<category>tube</category>
<category>algebra</category>
<category>gravitation</category>
</item>
<item>
<title>Algebras, regions, and observers. Algebras, regions, and observers Algebras, Regions, and Observers</title>
<description><span>In ordinary quantum field theory, one can define the algebra of observables in a given region in spacetime, but in the presence of gravity, it is expected that this notion ceases to be well-defined. A substitute that appears to make sense in the presence of gravity and that also is more operationally meaningful is to consider the algebra of observables along the timelike worldline of an observer. It is known that such an algebra can be defined in quantum field theory, and the timelike tube theorem of quantum field theory suggests that such an algebra is a good substitute for what in the absence of gravity is the algebra of a region. The static patch in de Sitter space is a concrete example in which it is useful to think in these terms and to explicitly incorporate an observer in the description.For the entire collection see [Zbl&nbsp;07836344].</span><br><span>In ordinary quantum field theory, one can define the algebra of observables in a given region in spacetime, but in the presence of gravity, it is expected that this notion ceases to be well-defined. A substitute that appears to make sense in the presence of gravity and that also is more operationally meaningful is to consider the algebra of observables along the timelike worldline of an observer. It is known that such an algebra can be defined in quantum field theory, and the timelike tube theorem of quantum field theory suggests that such an algebra is a good substitute for what in the absence of gravity is the algebra of a region. The static patch in de Sitter space is a concrete example in which it is useful to think in these terms and to explicitly incorporate an observer in the description.</span></description>
<link>https://inspirehep.net/literature/2638667</link>
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<pubDate>Tue, 07 Mar 2023 02:58:42 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>81T30</category>
<category>14N35</category>
<category>14J33</category>
<category>14J32</category>
<category>space: de Sitter</category>
<category>algebra</category>
<category>gravitation</category>
<category>space-time</category>
<category>tube</category>
</item>
<item>
<title>Analytic States in Quantum Field Theory on Curved Spacetimes Analytic states in quantum field theory on curved spacetimes</title>
<description><span>We discuss high energy properties of states for (possibly interacting) quantum fields in curved spacetimes. In particular, if the spacetime is real analytic, we show that an analogue of the timelike tube theorem and the Reeh–Schlieder property hold with respect to states satisfying a weak form of microlocal analyticity condition. The former means the von Neumann algebra of observables of a spacelike tube equals the von Neumann algebra of observables of a significantly bigger region that is obtained by deforming the boundary of the tube in a timelike manner. This generalizes theorems by Araki (Helv Phys Acta 36:132–139, 1963) and Borchers (Nuovo Cim (10) 19:787–793, 1961) to curved spacetimes.</span><br><span>We discuss high energy properties of states for (possibly interacting) quantum fields in curved spacetimes. In particular, if the spacetime is real analytic, we show that an analogue of the timelike tube theorem and the Reeh-Schlieder property hold with respect to states satisfying a weak form of microlocal analyticity condition. The former means the von Neumann algebra of observables of a spacelike tube equals the von Neumann algebra of observables of a significantly bigger region, that is obtained by deforming the boundary of the tube in a timelike manner. This generalizes theorems by Borchers and Araki to curved spacetimes.</span></description>
<link>https://inspirehep.net/literature/2629821</link>
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<pubDate>Tue, 07 Feb 2023 02:59:10 GMT</pubDate>
<author>Alexander Strohmaier (Leeds U., Math.), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>algebra: von Neumann</category>
<category>energy: high</category>
<category>space-time</category>
<category>tube</category>
<category>analytic properties</category>
</item>
<item>
<title>Algebras and States in JT Gravity</title>
<description><span>We analyze the algebra of boundary observables in canonically quantised JT gravity with or without matter. In the absence of matter, this algebra is commutative, generated by the ADM Hamiltonian. After coupling to a bulk quantum field theory, it becomes a highly noncommutative algebra of Type II$_\infty$ with a trivial center. As a result, density matrices and entropies on the boundary algebra are uniquely defined up to, respectively, a rescaling or shift. We show that this algebraic definition of entropy agrees with the usual replica trick definition computed using Euclidean path integrals. Unlike in previous arguments that focused on $\mathcal{O}(1)$ fluctuations to a black hole of specified mass, this Type II$_\infty$ algebra describes states at all temperatures or energies. We also consider the role of spacetime wormholes. One can try to define operators associated with wormholes that commute with the boundary algebra, but this fails in an instructive way. In a regulated version of the theory, wormholes and topology change can be incorporated perturbatively. The bulk Hilbert space $\mathcal{H}_\mathrm{bulk}$ that includes baby universe states is then much bigger than the space of states $\mathcal{H}_\mathrm{bdry}$ accessible to a boundary observer. However, to a boundary observer, every pure or mixed state on $\mathcal{H}_\mathrm{bulk}$ is equivalent to some pure state in $\mathcal{H}_\mathrm{bdry}$.</span></description>
<link>https://inspirehep.net/literature/2624347</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2624347</guid>
<pubDate>Thu, 19 Jan 2023 15:11:17 GMT</pubDate>
<author>Geoff Penington (Princeton, Inst. Advanced Study, UC, Berkeley), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>path integral: Euclidean</category>
<category>topology: transition</category>
<category>algebra: noncommutative</category>
<category>space-time: wormhole</category>
<category>entropy</category>
<category>field theory</category>
<category>gravitation</category>
<category>temperature</category>
<category>Hamiltonian</category>
<category>fluctuation</category>
<category>black hole</category>
<category>density matrix</category>
<category>quantization</category>
<category>Hilbert space</category>
<category>rescaling</category>
</item>
<item>
<title>A note on the canonical formalism for gravity A Note On The Canonical Formalism for Gravity</title>
<description><span>We describe a simple gauge-fixing that leads to a construction of a quantum Hilbert space for quantum gravity in an asymptotically Anti de&nbsp;Sitter spacetime, valid to all orders of perturbation theory. The construction is motivated by a relationship of the phase space of gravity in asymptotically Anti de&nbsp;Sitter spacetime to a cotangent bundle. We describe what is known about this relationship and some extensions that might plausibly be true. A key fact is that, under certain conditions, the Einstein Hamiltonian constraint equation can be viewed as a way to gauge fix the group of conformal rescalings of the metric of a Cauchy hypersurface. An analog of the procedure that we follow for Anti de&nbsp;Sitter gravity leads to standard results for a Klein–Gordon particle.</span><br><span>We describe a simple gauge-fixing that leads to a construction of a quantum Hilbert space for quantum gravity in an asymptotically Anti de Sitter spacetime, valid to all orders of perturbation theory. The construction is motivated by a relationship of the phase space of gravity in asymptotically Anti de Sitter spacetime to a cotangent bundle. We describe what is known about this relationship and some extensions that might plausibly be true. A key fact is that, under certain conditions, the Einstein Hamiltonian constraint equation can be viewed as a way to gauge fix the group of conformal rescalings of the metric of a Cauchy hypersurface. An analog of the procedure that we follow for Anti de Sitter gravity leads to standard results for a Klein-Gordon particle.</span></description>
<link>https://inspirehep.net/literature/2615434</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2615434</guid>
<pubDate>Mon, 19 Dec 2022 02:46:42 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>space-time: anti-de Sitter</category>
<category>rescaling: conformal</category>
<category>constraint: Hamiltonian</category>
<category>gravitation: anti-de Sitter</category>
<category>group: conformal</category>
<category>gauge fixing</category>
<category>quantum gravity</category>
<category>Hilbert space</category>
<category>perturbation theory</category>
<category>Einstein</category>
<category>phase space</category>
</item>
<item>
<title>Large N algebras and generalized entropy</title>
<description><span>We construct a Type II$_\infty$ von Neumann algebra that describes the large $N$ physics of single-trace operators in AdS/CFT in the microcanonical ensemble, where there is no need to include perturbative $1/N$ corrections. Using only the extrapolate dictionary, we show that the entropy of semiclassical states on this algebra is holographically dual to the generalized entropy of the black hole bifurcation surface. From a boundary perspective, this constitutes a derivation of a special case of the QES prescription without any use of Euclidean gravity or replicas; from a purely bulk perspective, it is a derivation of the quantum-corrected Bekenstein-Hawking formula as the entropy of an explicit algebra in the $G \to 0$ limit of Lorentzian effective field theory quantum gravity. In a limit where a black hole is first allowed to equilibrate and then is later potentially re-excited, we show that the generalized second law is a direct consequence of the monotonicity of the entropy of algebras under trace-preserving inclusions. Finally, by considering excitations that are separated by more than a scrambling time we construct a "free product" von Neumann algebra that describes the semiclassical physics of long wormholes supported by shocks. We compute Rényi entropies for this algebra and show that they are equal to a sum over saddles associated to quantum extremal surfaces in the wormhole. Surprisingly, however, the saddles associated to "bulge" quantum extremal surfaces contribute with a negative sign.</span></description>
<link>https://inspirehep.net/literature/2154670</link>
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<pubDate>Thu, 22 Sep 2022 03:36:55 GMT</pubDate>
<author>Venkatesa Chandrasekaran (Princeton, Inst. Advanced Study), Geoff Penington (Princeton, Inst. Advanced Study, UC, Berkeley), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>algebra: von Neumann</category>
<category>black hole: entropy</category>
<category>field theory: conformal</category>
<category>gravitation: Euclidean</category>
<category>duality: holography</category>
<category>entropy: semiclassical</category>
<category>surface</category>
<category>wormhole</category>
<category>excited state</category>
<category>quantum gravity</category>
<category>bifurcation</category>
<category>expansion 1/N</category>
<category>AdS/CFT correspondence</category>
<category>effective field theory</category>
</item>
<item>
<title>An algebra of observables for de Sitter space An Algebra of Observables for de Sitter Space</title>
<description><span>We describe an algebra of observables for a static patch in de Sitter space, with operators gravitationally dressed to the worldline of an observer. The algebra is a von Neumann algebra of Type II$_{1}$. There is a natural notion of entropy for a state of such an algebra. There is a maximum entropy state, which corresponds to empty de Sitter space, and the entropy of any semiclassical state of the Type II$_{1}$ algebras agrees, up to an additive constant independent of the state, with the expected generalized entropy S$_{gen}$ = (A/4G$_{N}$) + S$_{out}$. An arbitrary additive constant is present because of the renormalization that is involved in defining entropy for a Type II$_{1}$ algebra.</span><br><span>We describe an algebra of observables for a static patch in de Sitter space, with operators gravitationally dressed to the worldline of an observer. The algebra is a von Neumann algebra of Type II$_1$. There is a natural notion of entropy for a state of such an algebra. There is a maximum entropy state, which corresponds to empty de Sitter space, and the entropy of any semiclassical state of the Type II$_1$ algebras agrees, up to an additive constant independent of the state, with the expected generalized entropy $S_{\text{gen}}=(A/4G_N)+S_{\text{out}}$. An arbitrary additive constant is present because of the renormalization that is involved in defining entropy for a Type II$_1$ algebra.</span></description>
<link>https://inspirehep.net/literature/2099463</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2099463</guid>
<pubDate>Thu, 23 Jun 2022 03:30:04 GMT</pubDate>
<author>Venkatesa Chandrasekaran (Princeton, Inst. Advanced Study), Roberto Longo (Rome U., Tor Vergata), Geoff Penington (Princeton, Inst. Advanced Study, UC, Berkeley), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>Cosmological models</category>
<category>de Sitter space</category>
<category>space: de Sitter</category>
<category>algebra: von Neumann</category>
<category>entropy</category>
<category>semiclassical</category>
<category>gravitation</category>
<category>renormalization</category>
</item>
<item>
<title>A note on continuous entropy A note on continuous entropy</title>
<description><span>Von Neumann entropy has a natural extension to the case of an arbitrary semifinite von Neumann algebra, as was considered by I. E. Segal. We relate this entropy to the relative entropy and show that the entropy increase for an inclusion of von Neumann factors is bounded by the logarithm of the Jones index. The bound is optimal if the factors are infinite dimensional.</span><br><span>Von Neumann entropy has a natural extension to the case of an arbitrary semifinite von Neumann algebra, as was considered by I. E. Segal. We relate this entropy to the relative entropy and show that the entropy increase for an inclusion of von Neumann factors is bounded by the logarithm of the Jones index. The bound is optimal if the factors are infinite dimensional.</span></description>
<link>https://inspirehep.net/literature/2029393</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2029393</guid>
<pubDate>Tue, 08 Feb 2022 03:18:13 GMT</pubDate>
<author>Roberto Longo (Rome U., Tor Vergata), Edward Witten (Princeton, Inst. Advanced Study)</author>
</item>
<item>
<title>No ensemble averaging below the black hole threshold No Ensemble Averaging Below the Black Hole Threshold</title>
<description><span>In the AdS/CFT correspondence, amplitudes associated to connected bulk manifolds with disconnected boundaries have presented a longstanding mystery. A possible interpretation is that they reflect the effects of averaging over an ensemble of boundary theories. But in examples in dimension D ≥ 3, an appropriate ensemble of boundary theories does not exist. Here we sharpen the puzzle by identifying a class of “fixed energy” or “sub-threshold” observables that we claim do not show effects of ensemble averaging. These are amplitudes that involve states that are above the ground state by only a fixed amount in the large N limit, and in particular are far from being black hole states. To support our claim, we explore the example of D = 3, and show that connected solutions of Einstein’s equations with disconnected boundary never contribute to these observables. To demonstrate this requires some novel results about the renormalized volume of a hyperbolic three-manifold, which we prove using modern methods in hyperbolic geometry. Why then do any observables show apparent ensemble averaging? We propose that this reflects the chaotic nature of black hole physics and the fact that the Hilbert space describing a black hole does not have a large N limit.</span><br><span>In the AdS/CFT correspondence, amplitudes associated to connected bulk manifolds with disconnected boundaries have presented a longstanding mystery. A possible interpretation is that they reflect the effects of averaging over an ensemble of boundary theories. But in examples in dimension $D\geq 3$, an appropriate ensemble of boundary theories does not exist. Here we sharpen the puzzle by identifying a class of "sub-threshold" observables that we claim do not show effects of ensemble averaging. These are amplitudes that do not involve black hole states. To support our claim, we explore the example of $D=3$, and show that connected solutions of Einstein's equations with disconnected boundary never contribute to sub-threshold observables. To demonstrate this requires some novel results about the renormalized volume of a hyperbolic three-manifold, which we prove using modern methods in hyperbolic geometry. Why then do any observables show apparent ensemble averaging? We propose that this reflects the chaotic nature of black hole physics and the fact that the Hilbert space describing a black hole does not have a large $N$ limit.</span></description>
<link>https://inspirehep.net/literature/2026876</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2026876</guid>
<pubDate>Fri, 04 Feb 2022 07:49:06 GMT</pubDate>
<author>Jean-Marc Schlenker (Luxembourg U.), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>AdS-CFT Correspondence</category>
<category>Black Holes</category>
<category>Einstein equation: solution</category>
<category>field theory: conformal</category>
<category>black hole</category>
<category>geometry</category>
<category>Hilbert space</category>
<category>chaos</category>
<category>AdS/CFT correspondence</category>
</item>
<item>
<title>Gravity and the crossed product Gravity and the Crossed Product</title>
<description><span>Recently Leutheusser and Liu [1, 2] identified an emergent algebra of Type III$_{1}$ in the operator algebra of $ \mathcal{N} $ = 4 super Yang-Mills theory for large N. Here we describe some 1/N corrections to this picture and show that the emergent Type III$_{1}$ algebra becomes an algebra of Type II$_{∞}$. The Type II$_{∞}$ algebra is the crossed product of the Type III$_{1}$ algebra by its modular automorphism group. In the context of the emergent Type II$_{∞}$ algebra, the entropy of a black hole state is well-defined up to an additive constant, independent of the state. This is somewhat analogous to entropy in classical physics.</span><br><span>Recently Leutheusser and Liu [1,2] identified an emergent algebra of Type III$_1$ in the operator algebra of ${\mathcal N}=4$ super Yang-Mills theory for large $N$. Here we describe some $1/N$ corrections to this picture and show that the emergent Type III$_1$ algebra becomes an algebra of Type II$_\infty$. The Type II$_\infty$ algebra is the crossed product of the Type III$_1$ algebra by its modular automorphism group. In the context of the emergent Type II$_\infty$ algebra, the entropy of a black hole state is well-defined up to an additive constant, independent of the state. This is somewhat analogous to entropy in classical physics.</span></description>
<link>https://inspirehep.net/literature/1997150</link>
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<pubDate>Tue, 28 Dec 2021 02:51:58 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>1/N Expansion</category>
<category>AdS-CFT Correspondence</category>
<category>Black Holes</category>
<category>black hole: entropy</category>
<category>operator: algebra</category>
<category>Yang-Mills: supersymmetry</category>
<category>modular</category>
<category>supersymmetry: 4</category>
<category>expansion 1/N</category>
<category>nonperturbative</category>
<category>angular momentum</category>
<category>algebra: von Neumann</category>
</item>
<item>
<title>Why does quantum field theory in curved spacetime make sense? And what happens to the algebra of observables in the thermodynamic limit? Why Does Quan...</title>
<description><span>This article aims to explain some of the basic facts about the questions raised in the title, without the technical details that are available in the literature. We provide a gentle introduction to some rather classical results about quantum field theory in curved spacetime and about the thermodynamic limit of quantum statistical mechanics. We also briefly explain that these results have an analog in the large N limit of gauge theory.For the entire collection see [Zbl&nbsp;1515.81018].</span><br><span>This article aims to explain some of the basic facts about the questions raised in the title, without the technical details that are available in the literature. We provide a gentle introduction to some rather classical results about quantum field theory in curved spacetime and about the thermodynamic limit of quantum statistical mechanics. We also briefly explain that these results have an analog in the large N limit of gauge theory.</span></description>
<link>https://inspirehep.net/literature/1996057</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1996057</guid>
<pubDate>Thu, 23 Dec 2021 03:15:47 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>81Txx</category>
<category>statistics: quantum</category>
<category>space-time</category>
<category>thermodynamical</category>
<category>algebra: von Neumann</category>
<category>statistical mechanics</category>
<category>gauge field theory</category>
<category>expansion 1/N</category>
<category>introductory</category>
</item>
<item>
<title>A Note On Complex Spacetime Metrics</title>
<description><span>For various reasons, it seems necessary to include complex saddle points in the "Euclidean" path integral of General Relativity. But some sort of restriction on the allowed complex saddle points is needed to avoid various unphysical examples. In this article, a speculative proposal is made concerning a possible restriction on the allowed saddle points in the gravitational path integral. The proposal is motivated by recent work of Kontsevich and Segal on complex metrics in quantum field theory, and earlier work of Louko and Sorkin on topology change from a real time point of view.</span></description>
<link>https://inspirehep.net/literature/1967378</link>
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<pubDate>Mon, 15 Nov 2021 02:43:59 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>gravitation: path integral</category>
<category>space-time: complex</category>
<category>topology: transition</category>
<category>Euclidean</category>
<category>general relativity</category>
</item>
<item>
<title>On the black hole/string transition On the black hole/string transition</title>
<description><span>We discuss aspects of the possible transition between small black holes and highly excited fundamental strings. We focus on the connection between black holes and the self gravitating string solution of Horowitz and Polchinski. This solution is interesting because it has non-zero entropy at the classical level and it is natural to suspect that it might be continuously connected to the black hole. Surprisingly, we find a different behavior for heterotic and type II cases. For the type II case we find an obstruction to the idea that the two are connected as classical solutions of string theory, while no such obstruction exists for the heterotic case. We further provide a linear sigma model analysis that suggests a continuous connection for the heterotic case. We also describe a solution generating transformation that produces a charged version of the self gravitating string. This provides a fuzzball-like construction of near extremal configurations carrying fundamental string momentum and winding charges. We provide formulas which are exact in α′ relating the thermodynamic properties of the charged and the uncharged solutions.</span><br><span>We discuss aspects of the possible transition between small black holes and highly excited fundamental strings. We focus on the connection between black holes and the self gravitating string solution of Horowitz and Polchinski. This solution is interesting because it has non-zero entropy at the classical level and it is natural to suspect that it might be continuously connected to the black hole. Surprisingly, we find a different behavior for heterotic and type II cases. For the type II case we find an obstruction to the idea that the two are connected as classical solutions of string theory, while no such obstruction exists for the heterotic case. We further provide a linear sigma model analysis that suggests a continuous connection for the heterotic case. We also describe a solution generating transformation that produces a charged version of the self gravitating string. This provides a fuzzball-like construction of near extremal configurations carrying fundamental string momentum and winding charges. We provide formulas which are exact in $\alpha'$ relating the thermodynamic properties of the charged and the uncharged solutions.</span></description>
<link>https://inspirehep.net/literature/1923692</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1923692</guid>
<pubDate>Mon, 20 Sep 2021 02:56:51 GMT</pubDate>
<author>Yiming Chen (Princeton U.), Juan Maldacena (Princeton, Inst. Advanced Study), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>Black Holes</category>
<category>Black Holes in String Theory</category>
<category>Sigma Models</category>
<category>string: gravitation</category>
<category>black hole: string</category>
<category>sigma model: linear</category>
<category>string model: solution</category>
<category>heterotic</category>
<category>thermodynamical</category>
<category>entropy</category>
</item>
<item>
<title>Gauge Theory and the Analytic Form of the Geometric Langlands Program Gauge Theory and the Analytic Form of the Geometric Langlands Program</title>
<description><span>We present a gauge-theoretic interpretation of the “analytic” version of the geometric Langlands program, in which Hitchin Hamiltonians and Hecke operators are viewed as concrete operators acting on a Hilbert space of quantum states. The gauge theory ingredients required to understand this construction—such as electric–magnetic duality between Wilson and ’t Hooft line operators in four-dimensional gauge theory—are the same ones that enter in understanding via gauge theory the more familiar formulation of geometric Langlands, but now these ingredients are organized and applied in a novel fashion.</span><br><span>We present a gauge-theoretic interpretation of the "analytic" version of the geometric Langlands program, in which Hitchin Hamiltonians and Hecke operators are viewed as concrete operators acting on a Hilbert space of quantum states. The gauge theory ingredients required to understand this construction -- such as electric-magnetic duality between Wilson and 't Hooft line operators in four-dimensional gauge theory -- are the same ones that enter in understanding via gauge theory the more familiar formulation of geometric Langlands, but now these ingredients are organized and applied in a novel fashion.</span></description>
<link>https://inspirehep.net/literature/1876659</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1876659</guid>
<pubDate>Tue, 06 Jul 2021 03:15:30 GMT</pubDate>
<author>Davide Gaiotto (Perimeter Inst. Theor. Phys.), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>operator: Hecke</category>
<category>gauge field theory</category>
<category>Hilbert space</category>
<category>electromagnetic field: duality</category>
<category>Hamiltonian</category>
<category>geometry</category>
<category>Wilson loop</category>
<category>symplectic</category>
<category>WKB approximation</category>
</item>
<item>
<title>Matrix Models and Deformations of JT Gravity</title>
<description><span>Recently, it has been found that JT gravity, which is a two-dimensional theory with bulk action $ -\frac{1}{2}\int {\mathrm d}^2x \sqrt g\phi(R+2)$, is dual to a matrix model, that is, a random ensemble of quantum systems rather than a specific quantum mechanical system. In this article, we argue that a deformation of JT gravity with bulk action $ -\frac{1}{2}\int {\mathrm d}^2x \sqrt g(\phi R+W(\phi))$ is likewise dual to a matrix model. With a specific procedure for defining the path integral of the theory, we determine the density of eigenvalues of the dual matrix model. There is a simple answer if $W(0)=0$, and otherwise a rather complicated answer.</span></description>
<link>https://inspirehep.net/literature/1802756</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1802756</guid>
<pubDate>Thu, 25 Jun 2020 00:00:00 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>quantum gravity</category>
<category>JT gravity</category>
<category>matrix models</category>
<category>matrix model: duality</category>
<category>dimension: 2</category>
<category>gravitation</category>
<category>deformation</category>
<category>quantum mechanics</category>
<category>path integral</category>
</item>
<item>
<title>Averaging over Narain moduli space Averaging Over Narain Moduli Space</title>
<description><span>Recent developments involving JT gravity in two dimensions indicate that under some conditions, a gravitational path integral is dual to an average over an ensemble of boundary theories, rather than to a specific boundary theory. For an example in one dimension more, one would like to compare a random ensemble of two-dimensional CFT’s to Einstein gravity in three dimensions. But this is difficult. For a simpler problem, here we average over Narain’s family of two-dimensional CFT’s obtained by toroidal compactification. These theories are believed to be the most general ones with their central charges and abelian current algebra symmetries, so averaging over them means picking a random CFT with those properties. The average can be computed using the Siegel-Weil formula of number theory and has some properties suggestive of a bulk dual theory that would be an exotic theory of gravity in three dimensions. The bulk dual theory would be more like U(1)$^{2D}$ Chern-Simons theory than like Einstein gravity.</span><br><span>Recent developments involving JT gravity in two dimensions indicate that under some conditions, a gravitational path integral is dual to an average over an ensemble of boundary theories, rather than to a specific boundary theory. For an example in one dimension more, one would like to compare a random ensemble of two-dimensional CFT's to Einstein gravity in three dimensions. But this is difficult. For a simpler problem, here we average over Narain's family of two-dimensional CFT's obtained by toroidal compactification. These theories are believed to be the most general ones with their central charges and abelian current algebra symmetries, so averaging over them means picking a random CFT with those properties. The average can be computed using the Siegel-Weil formula of number theory and has some properties suggestive of a bulk dual theory that would be an exotic theory of gravity in three dimensions. The bulk dual theory would be more like $U(1)^{2D}$ Chern-Simons theory than like Einstein gravity.</span></description>
<link>https://inspirehep.net/literature/1800422</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1800422</guid>
<pubDate>Thu, 11 Jun 2020 00:00:00 GMT</pubDate>
<author>Alexander Maloney (McGill U.), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>AdS-CFT Correspondence</category>
<category>Conformal Field Theory</category>
<category>Gauge-gravity correspondence</category>
<category>dimension: 2</category>
<category>gravitation: path integral</category>
<category>compactification: torus</category>
<category>Chern-Simons term</category>
<category>current algebra</category>
<category>number theory</category>
<category>moduli space</category>
<category>AdS/CFT correspondence</category>
<category>gauge field theory: U(1)**N</category>
</item>
<item>
<title>Deformations of JT Gravity and Phase Transitions</title>
<description><span>We re-examine the black hole solutions in classical theories of dilaton gravity in two dimensions. We consider an arbitrary dilaton potential such that there are black hole solutions asymptotic at infinity to the nearly $\mathrm{AdS}_2$ solutions of JT gravity, and such that the black hole energy and entropy are bounded below. We show that if there is a black hole solution with negative specific heat at some temperature $T$, then at the same temperature there is a black hole solution with lower free energy and positive specific heat. As the temperature is increased from 0 to infinity, the black hole energy and entropy increase monotonically but not necessarily continuously; there can be first order phase transitions, similar to the Hawking-Page transition. These theories can also have solutions corresponding to closed universes.</span></description>
<link>https://inspirehep.net/literature/1799641</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1799641</guid>
<pubDate>Mon, 08 Jun 2020 00:00:00 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>black hole: energy</category>
<category>gravitation: dilaton</category>
<category>dilaton: potential</category>
<category>dimension: 2</category>
<category>temperature</category>
<category>critical phenomena</category>
<category>specific heat</category>
<category>entropy</category>
<category>anti-de Sitter</category>
<category>free energy</category>
<category>deformation</category>
</item>
<item>
<title>Exploration of the outer solar system with fast and small sailcraft</title>
<description><span>Two new interplanetary technologies have advanced in the past decade to the point where they may enable exciting, affordable missions that reach further and faster deep into the outer regions of our solar system: (i) small and capable interplanetary spacecraft and (ii) light-driven sails. Combination of these two technologies could drastically reduce travel times within the solar system. We discuss a new paradigm that involves small and fast moving sailcraft that could enable exploration of distant regions of the solar system much sooner and faster than previously considered. We present some of the exciting science objectives for these miniaturized intelligent space systems that could lead to transformational advancements in the space sciences in the coming decade.</span></description>
<link>https://inspirehep.net/literature/1797867</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1797867</guid>
<pubDate>Wed, 27 May 2020 00:00:00 GMT</pubDate>
<author>Slava G. Turyshev (Caltech, JPL), Peter Klupar (NASA, Ames), Abraham Loeb (Harvard U.), Zachary Manchester (Stanford U., Phys. Dept.), Kevin Parkin (NASA, Ames), Edward Witten (Princeton, Inst. Advanced Study), S. Pete Worden (NASA, Ames)</author>
</item>
<item>
<title>Searching for a Black Hole in the Outer Solar System</title>
<description><span>There are hints of a novel object ("Planet 9") with a mass $5-10$ $M_\oplus$ in the outer Solar System, at a distance of order 500 AU. If it is a relatively conventional planet, it can be found in telescopic searches. Alternatively, it has been suggested that this body might be a primordial black hole (PBH). In that case, conventional searches will fail. A possible alternative is to probe the gravitational field of this object using small, laser-launched spacecraft, like the ones envisioned in the Breakthrough Starshot project. With a velocity of order $.001~c$, such spacecraft can reach Planet 9 roughly a decade after launch and can discover it if they can report timing measurements accurate to $10^{-5}$ seconds back to Earth.</span></description>
<link>https://inspirehep.net/literature/1793411</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1793411</guid>
<pubDate>Thu, 30 Apr 2020 00:00:00 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>black hole: primordial</category>
<category>solar system</category>
<category>gravitation</category>
<category>quantum chromodynamics</category>
<category>dark matter: annihilation</category>
<category>acceleration</category>
<category>orbit</category>
<category>exotic</category>
<category>velocity</category>
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<item>
<title>Instantons and the Large N=4 Algebra</title>
<description><span>We investigate the differential geometry of the moduli space of instantons on ${\mathrm S}^3 \times {\mathrm S}^1$. Extending previous results, we show that a sigma-model with this target space can be expected to possess a large ${\mathcal N}=4$ superconformal symmetry, supporting speculations that this sigma-model may be dual to Type IIB superstring theory on $\mathrm{AdS}_3 \times {\mathrm S}^3 \times {\mathrm S}^3\times {\mathrm S}^1$.&nbsp; &nbsp;The sigma-model is parametrized by three integers -- the
rank of the gauge group, the instanton number, and a ``level'' (the integer coefficient of a topologically nontrivial $B$-field, analogous to a WZW level). These integers are expected to correspond to two five-brane charges and a one-brane charge.&nbsp; &nbsp;The sigma-model is weakly coupled when the level,&nbsp; conjecturally corresponding to one of the five-brane changes, becomes very large, keeping the other parameters fixed.&nbsp; The central charges of the large ${\mathcal N}=4$ algebra agree, at least semiclassically, with expectations from the duality.</span></description>
<link>https://inspirehep.net/literature/2812078</link>
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<pubDate>Wed, 31 Jul 2024 04:28:30 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
</item>
<item>
<title>Scale and Conformal Invariance in 2d Sigma Models, with an Application to N=4 Supersymmetry</title>
<description><span>By adapting previously known arguments concerning Ricci flow and the c-theorem, we give a direct proof that in a two-dimensional sigma-model with compact target space, scale invariance implies conformal invariance in perturbation theory. This argument, which applies to a general sigma-model constructed with a target space metric and B-field, is in accord with a more general proof in the literature that applies to arbitrary two-dimensional quantum field theories. Models with extended supersymmetry and a B-field are known to provide interesting test cases for the relation between scale invariance and conformal invariance in sigma-model perturbation theory. We give examples showing that in such models, the obstructions to conformal invariance suggested by general arguments can actually occur in models with target spaces that are not compact or complete. Thus compactness of the target space, or at least a suitable condition of completeness, is necessary as well as sufficient to ensure that scale invariance implies conformal invariance in models of this type.</span></description>
<link>https://inspirehep.net/literature/2782301</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2782301</guid>
<pubDate>Wed, 01 May 2024 03:53:57 GMT</pubDate>
<author>Georgios Papadopoulos (King's Coll. London, Dept. Math), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>invariance: conformal</category>
<category>invariance: scale</category>
<category>dimension: 2</category>
<category>supersymmetry</category>
<category>flow: Ricci</category>
<category>sigma model</category>
<category>perturbation theory</category>
<category>mathematical methods</category>
<category>space: compact</category>
</item>
<item>
<title>Liouville Theory: An Introduction to Rigorous Approaches</title>
<description><span>In recent years, a surprisingly direct and simple rigorous understanding of quantum Liouville theory has developed. We aim here to make this material more accessible to physicists working on quantum field theory.</span></description>
<link>https://inspirehep.net/literature/2773427</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2773427</guid>
<pubDate>Wed, 03 Apr 2024 03:50:18 GMT</pubDate>
<author>Sourav Chatterjee (Stanford U.), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>field theory: Liouville</category>
</item>
<item>
<title>A background-independent algebra in quantum gravity A Background Independent Algebra in Quantum Gravity</title>
<description><span>We propose an algebra of operators along an observer’s worldline as a background-independent algebra in quantum gravity. In that context, it is natural to think of the Hartle-Hawking no boundary state as a universal state of maximum entropy, and to define entropy in terms of the relative entropy with this state. In the case that the only spacetimes considered correspond to de Sitter vacua with different values of the cosmological constant, this definition leads to sensible results.</span><br><span>We propose an algebra of operators along an observer's worldline as a background-independent algebra in quantum gravity. In that context, it is natural to think of the Hartle-Hawking no boundary state as a universal state of maximum entropy, and to define entropy in terms of the relative entropy with this state. In the case that the only spacetimes considered correspond to de Sitter vacua with different values of the cosmological constant, this definition leads to sensible results.</span></description>
<link>https://inspirehep.net/literature/2686072</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2686072</guid>
<pubDate>Tue, 08 Aug 2023 08:29:45 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>Cosmological models</category>
<category>de Sitter space</category>
<category>operator: algebra</category>
<category>vacuum state: de Sitter</category>
<category>entropy</category>
<category>quantum gravity</category>
<category>cosmological constant</category>
<category>space-time</category>
<category>background</category>
</item>
<item>
<title>$ \mathcal{N} $ = 2 JT supergravity and matrix models $N=2$ JT Supergravity and Matrix Models $\mathcal{N}=2$ JT Supergravity and Matrix Models</title>
<description><span>Generalizing previous results for $ \mathcal{N} $ = 0 and $ \mathcal{N} $ = 1, we analyze $ \mathcal{N} $ = 2 JT supergravity on asymptotically AdS$_{2}$ spaces with arbitrary topology and show that this theory of gravity is dual, in a holographic sense, to a certain random matrix ensemble in which supermultiplets of different R-charge are statistically independent and each is described by its own $ \mathcal{N} $ = 2 random matrix ensemble. We also analyze the case with a time-reversal symmetry, either commuting or anticommuting with the R-charge. In order to compare supergravity to random matrix theory, we develop an $ \mathcal{N} $ = 2 analog of the recursion relations for Weil-Petersson volumes originally discovered by Mirzakhani in the bosonic case.</span><br><span>Generalizing previous results for $N=0$ and $N=1$, we analyze $N=2$ JT supergravity on asymptotically AdS${}_2$ spaces with arbitrary topology and show that this theory of gravity is dual, in a holographic sense, to a certain random matrix ensemble in which supermultiplets of different $R$-charge are statistically independent and each is described by its own $N=2$ random matrix ensemble. We also analyze the case with a time-reversal symmetry, either commuting or anticommuting with the $R$-charge. In order to compare supergravity to random matrix theory, we develop an $N=2$ analog of the recursion relations for Weil-Petersson volumes originally discovered by Mirzakhani in the bosonic case.</span></description>
<link>https://inspirehep.net/literature/2664145</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2664145</guid>
<pubDate>Thu, 01 Jun 2023 02:55:33 GMT</pubDate>
<author>Gustavo J. Turiaci (Princeton, Inst. Advanced Study, Washington U., Seattle), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>Black Holes</category>
<category>Extended Supersymmetry</category>
<category>Matrix Models</category>
<category>matrix model: random</category>
<category>time reversal: symmetry</category>
<category>supergravity: 2</category>
<category>duality: holography</category>
<category>topology</category>
<category>space: anti-de Sitter</category>
<category>dimension: 2</category>
<category>path integral</category>
<category>black hole</category>
</item>
<item>
<title>Anomalies and Nonsupersymmetric D-Branes</title>
<description><span>We revisit some aspects of D-brane theory from the point of view of anomalies. When the boundary condition on a worldsheet boson is flipped from Neumann to Dirichlet, worldsheet supersymmetry requires also reversing the sign of the boundary condition of the corresponding worldsheet fermion. This induces an anomaly which is a mod 2 anomaly in Type II superstring theory and a mod 8 anomaly in Type I superstring theory. The same anomaly also receives contributions from a sign in the sum over bulk spin structures (in Type IIA superstring theory), Chan-Paton factors of symplectic type (in Type I superstring theory), and Majorana fermions that propagate only on the worldsheet boundary. The need to cancel the anomaly accounts for many properties of supersymmetric and especially nonsupersymmetric D-branes in Type I and Type II superstring theory.</span></description>
<link>https://inspirehep.net/literature/2655986</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2655986</guid>
<pubDate>Wed, 03 May 2023 03:05:13 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>fermion: Majorana</category>
<category>anomaly</category>
<category>superstring</category>
<category>D-brane</category>
<category>boundary condition</category>
<category>structure</category>
<category>Chan-Paton factor</category>
<category>symplectic</category>
<category>spin</category>
</item>
<item>
<title>The Timelike Tube Theorem in Curved Spacetime The Timelike Tube Theorem in Curved Spacetime</title>
<description><span>The timelike tube theorem asserts that in quantum field theory without gravity, the algebra of observables in an open set ${\mathcal {U}}$ is the same as the corresponding algebra of observables in its “timelike envelope” ${\mathcal {E}}({\mathcal {U}})$, which is an open set that is in general larger. The theorem was originally proved in the 1960’s by Borchers and Araki for quantum fields in Minkowski space. Here we sketch the proof of a version of the theorem for quantum fields in a general real analytic spacetime. Details have appeared elsewhere.</span><br><span>The timelike tube theorem asserts that in quantum field theory without gravity, the algebra of observables in an open set U is the same as the corresponding algebra of observables in its ``timelike envelope'' E(U), which is an open set that is in general larger. The theorem was originally proved in the 1960's by Borchers and Araki for quantum fields in Minkowski space. Here we sketch the proof of a version of the theorem for quantum fields in a general real analytic spacetime. Details have appeared elsewhere.</span></description>
<link>https://inspirehep.net/literature/2646935</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2646935</guid>
<pubDate>Thu, 30 Mar 2023 03:03:37 GMT</pubDate>
<author>Alexander Strohmaier (Leeds U., Math.), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>space: Minkowski</category>
<category>space-time</category>
<category>tube</category>
<category>algebra</category>
<category>gravitation</category>
</item>
<item>
<title>Algebras, regions, and observers. Algebras, regions, and observers Algebras, Regions, and Observers</title>
<description><span>In ordinary quantum field theory, one can define the algebra of observables in a given region in spacetime, but in the presence of gravity, it is expected that this notion ceases to be well-defined. A substitute that appears to make sense in the presence of gravity and that also is more operationally meaningful is to consider the algebra of observables along the timelike worldline of an observer. It is known that such an algebra can be defined in quantum field theory, and the timelike tube theorem of quantum field theory suggests that such an algebra is a good substitute for what in the absence of gravity is the algebra of a region. The static patch in de Sitter space is a concrete example in which it is useful to think in these terms and to explicitly incorporate an observer in the description.For the entire collection see [Zbl&nbsp;07836344].</span><br><span>In ordinary quantum field theory, one can define the algebra of observables in a given region in spacetime, but in the presence of gravity, it is expected that this notion ceases to be well-defined. A substitute that appears to make sense in the presence of gravity and that also is more operationally meaningful is to consider the algebra of observables along the timelike worldline of an observer. It is known that such an algebra can be defined in quantum field theory, and the timelike tube theorem of quantum field theory suggests that such an algebra is a good substitute for what in the absence of gravity is the algebra of a region. The static patch in de Sitter space is a concrete example in which it is useful to think in these terms and to explicitly incorporate an observer in the description.</span></description>
<link>https://inspirehep.net/literature/2638667</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2638667</guid>
<pubDate>Tue, 07 Mar 2023 02:58:42 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>81T30</category>
<category>14N35</category>
<category>14J33</category>
<category>14J32</category>
<category>space: de Sitter</category>
<category>algebra</category>
<category>gravitation</category>
<category>space-time</category>
<category>tube</category>
</item>
<item>
<title>Analytic States in Quantum Field Theory on Curved Spacetimes Analytic states in quantum field theory on curved spacetimes</title>
<description><span>We discuss high energy properties of states for (possibly interacting) quantum fields in curved spacetimes. In particular, if the spacetime is real analytic, we show that an analogue of the timelike tube theorem and the Reeh–Schlieder property hold with respect to states satisfying a weak form of microlocal analyticity condition. The former means the von Neumann algebra of observables of a spacelike tube equals the von Neumann algebra of observables of a significantly bigger region that is obtained by deforming the boundary of the tube in a timelike manner. This generalizes theorems by Araki (Helv Phys Acta 36:132–139, 1963) and Borchers (Nuovo Cim (10) 19:787–793, 1961) to curved spacetimes.</span><br><span>We discuss high energy properties of states for (possibly interacting) quantum fields in curved spacetimes. In particular, if the spacetime is real analytic, we show that an analogue of the timelike tube theorem and the Reeh-Schlieder property hold with respect to states satisfying a weak form of microlocal analyticity condition. The former means the von Neumann algebra of observables of a spacelike tube equals the von Neumann algebra of observables of a significantly bigger region, that is obtained by deforming the boundary of the tube in a timelike manner. This generalizes theorems by Borchers and Araki to curved spacetimes.</span></description>
<link>https://inspirehep.net/literature/2629821</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2629821</guid>
<pubDate>Tue, 07 Feb 2023 02:59:10 GMT</pubDate>
<author>Alexander Strohmaier (Leeds U., Math.), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>algebra: von Neumann</category>
<category>energy: high</category>
<category>space-time</category>
<category>tube</category>
<category>analytic properties</category>
</item>
<item>
<title>Algebras and States in JT Gravity</title>
<description><span>We analyze the algebra of boundary observables in canonically quantised JT gravity with or without matter. In the absence of matter, this algebra is commutative, generated by the ADM Hamiltonian. After coupling to a bulk quantum field theory, it becomes a highly noncommutative algebra of Type II$_\infty$ with a trivial center. As a result, density matrices and entropies on the boundary algebra are uniquely defined up to, respectively, a rescaling or shift. We show that this algebraic definition of entropy agrees with the usual replica trick definition computed using Euclidean path integrals. Unlike in previous arguments that focused on $\mathcal{O}(1)$ fluctuations to a black hole of specified mass, this Type II$_\infty$ algebra describes states at all temperatures or energies. We also consider the role of spacetime wormholes. One can try to define operators associated with wormholes that commute with the boundary algebra, but this fails in an instructive way. In a regulated version of the theory, wormholes and topology change can be incorporated perturbatively. The bulk Hilbert space $\mathcal{H}_\mathrm{bulk}$ that includes baby universe states is then much bigger than the space of states $\mathcal{H}_\mathrm{bdry}$ accessible to a boundary observer. However, to a boundary observer, every pure or mixed state on $\mathcal{H}_\mathrm{bulk}$ is equivalent to some pure state in $\mathcal{H}_\mathrm{bdry}$.</span></description>
<link>https://inspirehep.net/literature/2624347</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2624347</guid>
<pubDate>Thu, 19 Jan 2023 15:11:17 GMT</pubDate>
<author>Geoff Penington (Princeton, Inst. Advanced Study, UC, Berkeley), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>path integral: Euclidean</category>
<category>topology: transition</category>
<category>algebra: noncommutative</category>
<category>space-time: wormhole</category>
<category>entropy</category>
<category>field theory</category>
<category>gravitation</category>
<category>temperature</category>
<category>Hamiltonian</category>
<category>fluctuation</category>
<category>black hole</category>
<category>density matrix</category>
<category>quantization</category>
<category>Hilbert space</category>
<category>rescaling</category>
</item>
<item>
<title>A note on the canonical formalism for gravity A Note On The Canonical Formalism for Gravity</title>
<description><span>We describe a simple gauge-fixing that leads to a construction of a quantum Hilbert space for quantum gravity in an asymptotically Anti de&nbsp;Sitter spacetime, valid to all orders of perturbation theory. The construction is motivated by a relationship of the phase space of gravity in asymptotically Anti de&nbsp;Sitter spacetime to a cotangent bundle. We describe what is known about this relationship and some extensions that might plausibly be true. A key fact is that, under certain conditions, the Einstein Hamiltonian constraint equation can be viewed as a way to gauge fix the group of conformal rescalings of the metric of a Cauchy hypersurface. An analog of the procedure that we follow for Anti de&nbsp;Sitter gravity leads to standard results for a Klein–Gordon particle.</span><br><span>We describe a simple gauge-fixing that leads to a construction of a quantum Hilbert space for quantum gravity in an asymptotically Anti de Sitter spacetime, valid to all orders of perturbation theory. The construction is motivated by a relationship of the phase space of gravity in asymptotically Anti de Sitter spacetime to a cotangent bundle. We describe what is known about this relationship and some extensions that might plausibly be true. A key fact is that, under certain conditions, the Einstein Hamiltonian constraint equation can be viewed as a way to gauge fix the group of conformal rescalings of the metric of a Cauchy hypersurface. An analog of the procedure that we follow for Anti de Sitter gravity leads to standard results for a Klein-Gordon particle.</span></description>
<link>https://inspirehep.net/literature/2615434</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2615434</guid>
<pubDate>Mon, 19 Dec 2022 02:46:42 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>space-time: anti-de Sitter</category>
<category>rescaling: conformal</category>
<category>constraint: Hamiltonian</category>
<category>gravitation: anti-de Sitter</category>
<category>group: conformal</category>
<category>gauge fixing</category>
<category>quantum gravity</category>
<category>Hilbert space</category>
<category>perturbation theory</category>
<category>Einstein</category>
<category>phase space</category>
</item>
<item>
<title>Large N algebras and generalized entropy</title>
<description><span>We construct a Type II$_\infty$ von Neumann algebra that describes the large $N$ physics of single-trace operators in AdS/CFT in the microcanonical ensemble, where there is no need to include perturbative $1/N$ corrections. Using only the extrapolate dictionary, we show that the entropy of semiclassical states on this algebra is holographically dual to the generalized entropy of the black hole bifurcation surface. From a boundary perspective, this constitutes a derivation of a special case of the QES prescription without any use of Euclidean gravity or replicas; from a purely bulk perspective, it is a derivation of the quantum-corrected Bekenstein-Hawking formula as the entropy of an explicit algebra in the $G \to 0$ limit of Lorentzian effective field theory quantum gravity. In a limit where a black hole is first allowed to equilibrate and then is later potentially re-excited, we show that the generalized second law is a direct consequence of the monotonicity of the entropy of algebras under trace-preserving inclusions. Finally, by considering excitations that are separated by more than a scrambling time we construct a "free product" von Neumann algebra that describes the semiclassical physics of long wormholes supported by shocks. We compute Rényi entropies for this algebra and show that they are equal to a sum over saddles associated to quantum extremal surfaces in the wormhole. Surprisingly, however, the saddles associated to "bulge" quantum extremal surfaces contribute with a negative sign.</span></description>
<link>https://inspirehep.net/literature/2154670</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2154670</guid>
<pubDate>Thu, 22 Sep 2022 03:36:55 GMT</pubDate>
<author>Venkatesa Chandrasekaran (Princeton, Inst. Advanced Study), Geoff Penington (Princeton, Inst. Advanced Study, UC, Berkeley), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>algebra: von Neumann</category>
<category>black hole: entropy</category>
<category>field theory: conformal</category>
<category>gravitation: Euclidean</category>
<category>duality: holography</category>
<category>entropy: semiclassical</category>
<category>surface</category>
<category>wormhole</category>
<category>excited state</category>
<category>quantum gravity</category>
<category>bifurcation</category>
<category>expansion 1/N</category>
<category>AdS/CFT correspondence</category>
<category>effective field theory</category>
</item>
<item>
<title>An algebra of observables for de Sitter space An Algebra of Observables for de Sitter Space</title>
<description><span>We describe an algebra of observables for a static patch in de Sitter space, with operators gravitationally dressed to the worldline of an observer. The algebra is a von Neumann algebra of Type II$_{1}$. There is a natural notion of entropy for a state of such an algebra. There is a maximum entropy state, which corresponds to empty de Sitter space, and the entropy of any semiclassical state of the Type II$_{1}$ algebras agrees, up to an additive constant independent of the state, with the expected generalized entropy S$_{gen}$ = (A/4G$_{N}$) + S$_{out}$. An arbitrary additive constant is present because of the renormalization that is involved in defining entropy for a Type II$_{1}$ algebra.</span><br><span>We describe an algebra of observables for a static patch in de Sitter space, with operators gravitationally dressed to the worldline of an observer. The algebra is a von Neumann algebra of Type II$_1$. There is a natural notion of entropy for a state of such an algebra. There is a maximum entropy state, which corresponds to empty de Sitter space, and the entropy of any semiclassical state of the Type II$_1$ algebras agrees, up to an additive constant independent of the state, with the expected generalized entropy $S_{\text{gen}}=(A/4G_N)+S_{\text{out}}$. An arbitrary additive constant is present because of the renormalization that is involved in defining entropy for a Type II$_1$ algebra.</span></description>
<link>https://inspirehep.net/literature/2099463</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2099463</guid>
<pubDate>Thu, 23 Jun 2022 03:30:04 GMT</pubDate>
<author>Venkatesa Chandrasekaran (Princeton, Inst. Advanced Study), Roberto Longo (Rome U., Tor Vergata), Geoff Penington (Princeton, Inst. Advanced Study, UC, Berkeley), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>Cosmological models</category>
<category>de Sitter space</category>
<category>space: de Sitter</category>
<category>algebra: von Neumann</category>
<category>entropy</category>
<category>semiclassical</category>
<category>gravitation</category>
<category>renormalization</category>
</item>
<item>
<title>A note on continuous entropy A note on continuous entropy</title>
<description><span>Von Neumann entropy has a natural extension to the case of an arbitrary semifinite von Neumann algebra, as was considered by I. E. Segal. We relate this entropy to the relative entropy and show that the entropy increase for an inclusion of von Neumann factors is bounded by the logarithm of the Jones index. The bound is optimal if the factors are infinite dimensional.</span><br><span>Von Neumann entropy has a natural extension to the case of an arbitrary semifinite von Neumann algebra, as was considered by I. E. Segal. We relate this entropy to the relative entropy and show that the entropy increase for an inclusion of von Neumann factors is bounded by the logarithm of the Jones index. The bound is optimal if the factors are infinite dimensional.</span></description>
<link>https://inspirehep.net/literature/2029393</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2029393</guid>
<pubDate>Tue, 08 Feb 2022 03:18:13 GMT</pubDate>
<author>Roberto Longo (Rome U., Tor Vergata), Edward Witten (Princeton, Inst. Advanced Study)</author>
</item>
<item>
<title>No ensemble averaging below the black hole threshold No Ensemble Averaging Below the Black Hole Threshold</title>
<description><span>In the AdS/CFT correspondence, amplitudes associated to connected bulk manifolds with disconnected boundaries have presented a longstanding mystery. A possible interpretation is that they reflect the effects of averaging over an ensemble of boundary theories. But in examples in dimension D ≥ 3, an appropriate ensemble of boundary theories does not exist. Here we sharpen the puzzle by identifying a class of “fixed energy” or “sub-threshold” observables that we claim do not show effects of ensemble averaging. These are amplitudes that involve states that are above the ground state by only a fixed amount in the large N limit, and in particular are far from being black hole states. To support our claim, we explore the example of D = 3, and show that connected solutions of Einstein’s equations with disconnected boundary never contribute to these observables. To demonstrate this requires some novel results about the renormalized volume of a hyperbolic three-manifold, which we prove using modern methods in hyperbolic geometry. Why then do any observables show apparent ensemble averaging? We propose that this reflects the chaotic nature of black hole physics and the fact that the Hilbert space describing a black hole does not have a large N limit.</span><br><span>In the AdS/CFT correspondence, amplitudes associated to connected bulk manifolds with disconnected boundaries have presented a longstanding mystery. A possible interpretation is that they reflect the effects of averaging over an ensemble of boundary theories. But in examples in dimension $D\geq 3$, an appropriate ensemble of boundary theories does not exist. Here we sharpen the puzzle by identifying a class of "sub-threshold" observables that we claim do not show effects of ensemble averaging. These are amplitudes that do not involve black hole states. To support our claim, we explore the example of $D=3$, and show that connected solutions of Einstein's equations with disconnected boundary never contribute to sub-threshold observables. To demonstrate this requires some novel results about the renormalized volume of a hyperbolic three-manifold, which we prove using modern methods in hyperbolic geometry. Why then do any observables show apparent ensemble averaging? We propose that this reflects the chaotic nature of black hole physics and the fact that the Hilbert space describing a black hole does not have a large $N$ limit.</span></description>
<link>https://inspirehep.net/literature/2026876</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2026876</guid>
<pubDate>Fri, 04 Feb 2022 07:49:06 GMT</pubDate>
<author>Jean-Marc Schlenker (Luxembourg U.), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>AdS-CFT Correspondence</category>
<category>Black Holes</category>
<category>Einstein equation: solution</category>
<category>field theory: conformal</category>
<category>black hole</category>
<category>geometry</category>
<category>Hilbert space</category>
<category>chaos</category>
<category>AdS/CFT correspondence</category>
</item>
<item>
<title>Gravity and the crossed product Gravity and the Crossed Product</title>
<description><span>Recently Leutheusser and Liu [1, 2] identified an emergent algebra of Type III$_{1}$ in the operator algebra of $ \mathcal{N} $ = 4 super Yang-Mills theory for large N. Here we describe some 1/N corrections to this picture and show that the emergent Type III$_{1}$ algebra becomes an algebra of Type II$_{∞}$. The Type II$_{∞}$ algebra is the crossed product of the Type III$_{1}$ algebra by its modular automorphism group. In the context of the emergent Type II$_{∞}$ algebra, the entropy of a black hole state is well-defined up to an additive constant, independent of the state. This is somewhat analogous to entropy in classical physics.</span><br><span>Recently Leutheusser and Liu [1,2] identified an emergent algebra of Type III$_1$ in the operator algebra of ${\mathcal N}=4$ super Yang-Mills theory for large $N$. Here we describe some $1/N$ corrections to this picture and show that the emergent Type III$_1$ algebra becomes an algebra of Type II$_\infty$. The Type II$_\infty$ algebra is the crossed product of the Type III$_1$ algebra by its modular automorphism group. In the context of the emergent Type II$_\infty$ algebra, the entropy of a black hole state is well-defined up to an additive constant, independent of the state. This is somewhat analogous to entropy in classical physics.</span></description>
<link>https://inspirehep.net/literature/1997150</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1997150</guid>
<pubDate>Tue, 28 Dec 2021 02:51:58 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>1/N Expansion</category>
<category>AdS-CFT Correspondence</category>
<category>Black Holes</category>
<category>black hole: entropy</category>
<category>operator: algebra</category>
<category>Yang-Mills: supersymmetry</category>
<category>modular</category>
<category>supersymmetry: 4</category>
<category>expansion 1/N</category>
<category>nonperturbative</category>
<category>angular momentum</category>
<category>algebra: von Neumann</category>
</item>
<item>
<title>Why does quantum field theory in curved spacetime make sense? And what happens to the algebra of observables in the thermodynamic limit? Why Does Quan...</title>
<description><span>This article aims to explain some of the basic facts about the questions raised in the title, without the technical details that are available in the literature. We provide a gentle introduction to some rather classical results about quantum field theory in curved spacetime and about the thermodynamic limit of quantum statistical mechanics. We also briefly explain that these results have an analog in the large N limit of gauge theory.For the entire collection see [Zbl&nbsp;1515.81018].</span><br><span>This article aims to explain some of the basic facts about the questions raised in the title, without the technical details that are available in the literature. We provide a gentle introduction to some rather classical results about quantum field theory in curved spacetime and about the thermodynamic limit of quantum statistical mechanics. We also briefly explain that these results have an analog in the large N limit of gauge theory.</span></description>
<link>https://inspirehep.net/literature/1996057</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1996057</guid>
<pubDate>Thu, 23 Dec 2021 03:15:47 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>81Txx</category>
<category>statistics: quantum</category>
<category>space-time</category>
<category>thermodynamical</category>
<category>algebra: von Neumann</category>
<category>statistical mechanics</category>
<category>gauge field theory</category>
<category>expansion 1/N</category>
<category>introductory</category>
</item>
<item>
<title>A Note On Complex Spacetime Metrics</title>
<description><span>For various reasons, it seems necessary to include complex saddle points in the "Euclidean" path integral of General Relativity. But some sort of restriction on the allowed complex saddle points is needed to avoid various unphysical examples. In this article, a speculative proposal is made concerning a possible restriction on the allowed saddle points in the gravitational path integral. The proposal is motivated by recent work of Kontsevich and Segal on complex metrics in quantum field theory, and earlier work of Louko and Sorkin on topology change from a real time point of view.</span></description>
<link>https://inspirehep.net/literature/1967378</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1967378</guid>
<pubDate>Mon, 15 Nov 2021 02:43:59 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>gravitation: path integral</category>
<category>space-time: complex</category>
<category>topology: transition</category>
<category>Euclidean</category>
<category>general relativity</category>
</item>
<item>
<title>On the black hole/string transition On the black hole/string transition</title>
<description><span>We discuss aspects of the possible transition between small black holes and highly excited fundamental strings. We focus on the connection between black holes and the self gravitating string solution of Horowitz and Polchinski. This solution is interesting because it has non-zero entropy at the classical level and it is natural to suspect that it might be continuously connected to the black hole. Surprisingly, we find a different behavior for heterotic and type II cases. For the type II case we find an obstruction to the idea that the two are connected as classical solutions of string theory, while no such obstruction exists for the heterotic case. We further provide a linear sigma model analysis that suggests a continuous connection for the heterotic case. We also describe a solution generating transformation that produces a charged version of the self gravitating string. This provides a fuzzball-like construction of near extremal configurations carrying fundamental string momentum and winding charges. We provide formulas which are exact in α′ relating the thermodynamic properties of the charged and the uncharged solutions.</span><br><span>We discuss aspects of the possible transition between small black holes and highly excited fundamental strings. We focus on the connection between black holes and the self gravitating string solution of Horowitz and Polchinski. This solution is interesting because it has non-zero entropy at the classical level and it is natural to suspect that it might be continuously connected to the black hole. Surprisingly, we find a different behavior for heterotic and type II cases. For the type II case we find an obstruction to the idea that the two are connected as classical solutions of string theory, while no such obstruction exists for the heterotic case. We further provide a linear sigma model analysis that suggests a continuous connection for the heterotic case. We also describe a solution generating transformation that produces a charged version of the self gravitating string. This provides a fuzzball-like construction of near extremal configurations carrying fundamental string momentum and winding charges. We provide formulas which are exact in $\alpha'$ relating the thermodynamic properties of the charged and the uncharged solutions.</span></description>
<link>https://inspirehep.net/literature/1923692</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1923692</guid>
<pubDate>Mon, 20 Sep 2021 02:56:51 GMT</pubDate>
<author>Yiming Chen (Princeton U.), Juan Maldacena (Princeton, Inst. Advanced Study), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>Black Holes</category>
<category>Black Holes in String Theory</category>
<category>Sigma Models</category>
<category>string: gravitation</category>
<category>black hole: string</category>
<category>sigma model: linear</category>
<category>string model: solution</category>
<category>heterotic</category>
<category>thermodynamical</category>
<category>entropy</category>
</item>
<item>
<title>Gauge Theory and the Analytic Form of the Geometric Langlands Program Gauge Theory and the Analytic Form of the Geometric Langlands Program</title>
<description><span>We present a gauge-theoretic interpretation of the “analytic” version of the geometric Langlands program, in which Hitchin Hamiltonians and Hecke operators are viewed as concrete operators acting on a Hilbert space of quantum states. The gauge theory ingredients required to understand this construction—such as electric–magnetic duality between Wilson and ’t Hooft line operators in four-dimensional gauge theory—are the same ones that enter in understanding via gauge theory the more familiar formulation of geometric Langlands, but now these ingredients are organized and applied in a novel fashion.</span><br><span>We present a gauge-theoretic interpretation of the "analytic" version of the geometric Langlands program, in which Hitchin Hamiltonians and Hecke operators are viewed as concrete operators acting on a Hilbert space of quantum states. The gauge theory ingredients required to understand this construction -- such as electric-magnetic duality between Wilson and 't Hooft line operators in four-dimensional gauge theory -- are the same ones that enter in understanding via gauge theory the more familiar formulation of geometric Langlands, but now these ingredients are organized and applied in a novel fashion.</span></description>
<link>https://inspirehep.net/literature/1876659</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1876659</guid>
<pubDate>Tue, 06 Jul 2021 03:15:30 GMT</pubDate>
<author>Davide Gaiotto (Perimeter Inst. Theor. Phys.), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>operator: Hecke</category>
<category>gauge field theory</category>
<category>Hilbert space</category>
<category>electromagnetic field: duality</category>
<category>Hamiltonian</category>
<category>geometry</category>
<category>Wilson loop</category>
<category>symplectic</category>
<category>WKB approximation</category>
</item>
<item>
<title>Matrix Models and Deformations of JT Gravity</title>
<description><span>Recently, it has been found that JT gravity, which is a two-dimensional theory with bulk action $ -\frac{1}{2}\int {\mathrm d}^2x \sqrt g\phi(R+2)$, is dual to a matrix model, that is, a random ensemble of quantum systems rather than a specific quantum mechanical system. In this article, we argue that a deformation of JT gravity with bulk action $ -\frac{1}{2}\int {\mathrm d}^2x \sqrt g(\phi R+W(\phi))$ is likewise dual to a matrix model. With a specific procedure for defining the path integral of the theory, we determine the density of eigenvalues of the dual matrix model. There is a simple answer if $W(0)=0$, and otherwise a rather complicated answer.</span></description>
<link>https://inspirehep.net/literature/1802756</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1802756</guid>
<pubDate>Thu, 25 Jun 2020 00:00:00 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>quantum gravity</category>
<category>JT gravity</category>
<category>matrix models</category>
<category>matrix model: duality</category>
<category>dimension: 2</category>
<category>gravitation</category>
<category>deformation</category>
<category>quantum mechanics</category>
<category>path integral</category>
</item>
<item>
<title>Averaging over Narain moduli space Averaging Over Narain Moduli Space</title>
<description><span>Recent developments involving JT gravity in two dimensions indicate that under some conditions, a gravitational path integral is dual to an average over an ensemble of boundary theories, rather than to a specific boundary theory. For an example in one dimension more, one would like to compare a random ensemble of two-dimensional CFT’s to Einstein gravity in three dimensions. But this is difficult. For a simpler problem, here we average over Narain’s family of two-dimensional CFT’s obtained by toroidal compactification. These theories are believed to be the most general ones with their central charges and abelian current algebra symmetries, so averaging over them means picking a random CFT with those properties. The average can be computed using the Siegel-Weil formula of number theory and has some properties suggestive of a bulk dual theory that would be an exotic theory of gravity in three dimensions. The bulk dual theory would be more like U(1)$^{2D}$ Chern-Simons theory than like Einstein gravity.</span><br><span>Recent developments involving JT gravity in two dimensions indicate that under some conditions, a gravitational path integral is dual to an average over an ensemble of boundary theories, rather than to a specific boundary theory. For an example in one dimension more, one would like to compare a random ensemble of two-dimensional CFT's to Einstein gravity in three dimensions. But this is difficult. For a simpler problem, here we average over Narain's family of two-dimensional CFT's obtained by toroidal compactification. These theories are believed to be the most general ones with their central charges and abelian current algebra symmetries, so averaging over them means picking a random CFT with those properties. The average can be computed using the Siegel-Weil formula of number theory and has some properties suggestive of a bulk dual theory that would be an exotic theory of gravity in three dimensions. The bulk dual theory would be more like $U(1)^{2D}$ Chern-Simons theory than like Einstein gravity.</span></description>
<link>https://inspirehep.net/literature/1800422</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1800422</guid>
<pubDate>Thu, 11 Jun 2020 00:00:00 GMT</pubDate>
<author>Alexander Maloney (McGill U.), Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>AdS-CFT Correspondence</category>
<category>Conformal Field Theory</category>
<category>Gauge-gravity correspondence</category>
<category>dimension: 2</category>
<category>gravitation: path integral</category>
<category>compactification: torus</category>
<category>Chern-Simons term</category>
<category>current algebra</category>
<category>number theory</category>
<category>moduli space</category>
<category>AdS/CFT correspondence</category>
<category>gauge field theory: U(1)**N</category>
</item>
<item>
<title>Deformations of JT Gravity and Phase Transitions</title>
<description><span>We re-examine the black hole solutions in classical theories of dilaton gravity in two dimensions. We consider an arbitrary dilaton potential such that there are black hole solutions asymptotic at infinity to the nearly $\mathrm{AdS}_2$ solutions of JT gravity, and such that the black hole energy and entropy are bounded below. We show that if there is a black hole solution with negative specific heat at some temperature $T$, then at the same temperature there is a black hole solution with lower free energy and positive specific heat. As the temperature is increased from 0 to infinity, the black hole energy and entropy increase monotonically but not necessarily continuously; there can be first order phase transitions, similar to the Hawking-Page transition. These theories can also have solutions corresponding to closed universes.</span></description>
<link>https://inspirehep.net/literature/1799641</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1799641</guid>
<pubDate>Mon, 08 Jun 2020 00:00:00 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>black hole: energy</category>
<category>gravitation: dilaton</category>
<category>dilaton: potential</category>
<category>dimension: 2</category>
<category>temperature</category>
<category>critical phenomena</category>
<category>specific heat</category>
<category>entropy</category>
<category>anti-de Sitter</category>
<category>free energy</category>
<category>deformation</category>
</item>
<item>
<title>Exploration of the outer solar system with fast and small sailcraft</title>
<description><span>Two new interplanetary technologies have advanced in the past decade to the point where they may enable exciting, affordable missions that reach further and faster deep into the outer regions of our solar system: (i) small and capable interplanetary spacecraft and (ii) light-driven sails. Combination of these two technologies could drastically reduce travel times within the solar system. We discuss a new paradigm that involves small and fast moving sailcraft that could enable exploration of distant regions of the solar system much sooner and faster than previously considered. We present some of the exciting science objectives for these miniaturized intelligent space systems that could lead to transformational advancements in the space sciences in the coming decade.</span></description>
<link>https://inspirehep.net/literature/1797867</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1797867</guid>
<pubDate>Wed, 27 May 2020 00:00:00 GMT</pubDate>
<author>Slava G. Turyshev (Caltech, JPL), Peter Klupar (NASA, Ames), Abraham Loeb (Harvard U.), Zachary Manchester (Stanford U., Phys. Dept.), Kevin Parkin (NASA, Ames), Edward Witten (Princeton, Inst. Advanced Study), S. Pete Worden (NASA, Ames)</author>
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<title>Searching for a Black Hole in the Outer Solar System</title>
<description><span>There are hints of a novel object ("Planet 9") with a mass $5-10$ $M_\oplus$ in the outer Solar System, at a distance of order 500 AU. If it is a relatively conventional planet, it can be found in telescopic searches. Alternatively, it has been suggested that this body might be a primordial black hole (PBH). In that case, conventional searches will fail. A possible alternative is to probe the gravitational field of this object using small, laser-launched spacecraft, like the ones envisioned in the Breakthrough Starshot project. With a velocity of order $.001~c$, such spacecraft can reach Planet 9 roughly a decade after launch and can discover it if they can report timing measurements accurate to $10^{-5}$ seconds back to Earth.</span></description>
<link>https://inspirehep.net/literature/1793411</link>
<guid isPermaLink="false">https://inspirehep.net/literature/1793411</guid>
<pubDate>Thu, 30 Apr 2020 00:00:00 GMT</pubDate>
<author>Edward Witten (Princeton, Inst. Advanced Study)</author>
<category>black hole: primordial</category>
<category>solar system</category>
<category>gravitation</category>
<category>quantum chromodynamics</category>
<category>dark matter: annihilation</category>
<category>acceleration</category>
<category>orbit</category>
<category>exotic</category>
<category>velocity</category>
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<title>Image of the Kerr-Newman black hole surrounded by a thin accretion disk</title>
<description><span>The image of a Kerr-Newman (KN) black hole (BH) surrounded by a thin accretion disk is derived. By employing elliptic integrals and ray-tracing methods, we analyze photon trajectories around the KN BH. At low observation inclination angles, the secondary image of particles is embedded within the primary image. However, as the inclination increases, the primary and secondary images separate, forming a hat-like structure. The spin and charge of the BH, along with the observer's inclination angle, affect the image's asymmetry and the distortion of the inner shadow. To investigate the redshift distribution on the accretion disk, we extended the inner boundary of the accretion disk to the event horizon. The results show that the redshift distribution is significantly influenced by the observation inclination angle. Furthermore, we conducted a detailed analysis of the KN BH image using fisheye camera ray-tracing techniques and found that the optical appearance and intensity distribution of the BH vary at different observation frequencies (specifically at 230GHz and 86GHz). We also examined differences in intensity distribution for prograde and retrograde accretion disk scenarios. Comparing observational at the two frequencies, we found that both the total intensity and peak intensity at 86GHz are higher than those at 230GHz.</span></description>
<link>https://inspirehep.net/literature/2847560</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847560</guid>
<pubDate>Wed, 13 Nov 2024 04:36:04 GMT</pubDate>
<author>Sen Guo, Yu-Xiang Huang, En-Wei Liang, Yu Liang, Qing-Quan Jiang, Kai Lin</author>
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<title>Holographic multipartite entanglement from the upper bound of $n$-partite information</title>
<description><span>To analyze the holographic multipartite entanglement structure, we study the upper bound for holographic $n$-partite information $(-1)^n I_n$ that $n-1$ fixed boundary subregions participate together with an arbitrary region $E$. %In general cases, we could find regions $E$ that make $I_n$ approach the upper bound. For $n=3$, we show that the upper bound of $-I_3$ is given by a quantity that we name the entanglement of state-constrained purification $EoSP(A:B)$. For $n\geq4$, we find that the upper bound of $I_n$ is finite in holographic CFT$_{1+1}$ but has UV divergences in higher dimensions, which reveals a fundamental difference in the entanglement structure in different dimensions. When $(-1)^n I_n$ reaches the information-theoretical upper bound, we argue that \( I_n \) fully accounts for multipartite global entanglement in these upper bound critical points, in contrast to usual cases where $I_n$ is not a perfect measure for multipartite entanglement. We further show that these results suggest that fewer-partite entanglement fully emerges from more-partite entanglement, and any $n-1$ distant regions are fully $n$-partite entangling in higher dimensions.</span></description>
<link>https://inspirehep.net/literature/2847487</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847487</guid>
<pubDate>Wed, 13 Nov 2024 04:26:13 GMT</pubDate>
<author>Xin-Xiang Ju (Beijing, GUCAS), Wen-Bin Pan (Beijing, Inst. High Energy Phys., Beijing, GUCAS), Ya-Wen Sun (Beijing, GUCAS, Beijing, KITPC), Yang Zhao (Beijing, GUCAS)</author>
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<title>Primordial black holes and induced gravitational waves from logarithmic non-Gaussianity</title>
<description><span>We investigate the formation of primordial black hole (PBH) based on numerical relativity simulations and peak theory as well as the corresponding scalar induced gravitational wave (SIGW) signals in the presence of \emph{logarithmic non-Gaussianities} which has recently been confirmed in a wide class of inflation models. Through numerical calculations, we find certain parameter spaces of the critical thresholds for the type A PBH formation and reveal a maximum critical threshold value. We also find that there is a region where no PBH is produced from type II fluctuations contrary to a previous study. We then confirm that SIGW signals originated from the logarithmic non-Gaussianity are detectable in the Laser Interferometer Space Antenna if PBHs account for whole dark matter. Finally, we discuss the SIGW interpretation of the nHz stochastic gravitational wave background reported by the recent pulsar timing array observations. We find that PBH overproduction is a serious problem for most of the parameter space, while this tension might still be alleviated in the non-perturbative regime.</span></description>
<link>https://inspirehep.net/literature/2847486</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847486</guid>
<pubDate>Wed, 13 Nov 2024 04:25:36 GMT</pubDate>
<author>Ryoto Inui (Nagoya U.), Cristian Joana (Beijing, KITPC), Hayato Motohashi (Kogakuin U.), Shi Pi (Beijing, KITPC, Peking U., CHEP, Tokyo U., IPMU), Yuichiro Tada (Nagoya U., Nagoya U., ISEE), Shuichiro Yokoyama (Nagoya U., Tokyo U., IPMU, KMI, Nagoya)</author>
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<title>Studying KARMA (Kerr And Relativistic Matter Around)</title>
<description><span>We construct series of solutions for the Kerr-type rotating black hole with non-trivial matter in flat and (A)dS backgrounds. Symmetry arguments and singularity analysis in the proposed black hole models fix the free parameters of the solutions, and the study of popular energy conditions makes it possible to impose constraints on configuration and field content of external matter. The resulted geometry of spacetimes is featured by a special type singularity in the north and south pole directions, inducing the bipolar outflow of particles from black holes. As a step toward the construction of a non-stationary rotating black hole solution in the presence of matter, we explore the zero angular momentum limit of the constructed metrics. The use of the Eddington-Finkelstein coordinates allows us to find a generalization of the proposed construction to the Vaidya-type black hole. Finally, employing the Newman-Janis algorithm, we find the corresponding generalization of the Kerr-Vaidya black hole solution.</span></description>
<link>https://inspirehep.net/literature/2847470</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847470</guid>
<pubDate>Wed, 13 Nov 2024 04:23:36 GMT</pubDate>
<author>A.J. Nurmagambetov (Cracow, INP, Kharkov, KIPT, Kharkov Natl. U., Usikov Inst. Radio Phys. Electr., Kharkov)</author>
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<title>Primordial Black Hole Reformation in the Early Universe</title>
<description><span>Primordial black holes (PBH) can arise in a wide range of scenarios, from inflation to first-order phase transitions. Light PBHs, such as those produced during preheating or at the GUT scale, could induce an early matter-dominated phase given a moderate initial abundance. During the early matter-domination, the growth of initial PBH density perturbations can trigger collapse on horizon scales, producing much heavier PBHs. While the remaining original PBHs evaporate and reheat the Universe, these massive reformed PBHs survive for an extended period of time, producing potentially observable signatures at the present. We study this PBH reformation scenario and show that those reformed PBHs can emit significant quantities of gamma rays detectable by the next generation of experiments. The rapid reheating after matter domination generates a coincident stochastic gravitational wave background, which could be within range of the upcoming CMB-S4 experiment. The PBH reformation scenario provides an intriguing possibility of decoupling the current PBH population and the initial formation mechanism from early Universe physics, while providing opportunities for observation through multi-messenger astronomy.</span></description>
<link>https://inspirehep.net/literature/2847469</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847469</guid>
<pubDate>Wed, 13 Nov 2024 04:23:35 GMT</pubDate>
<author>Taehun Kim (Korea Inst. Advanced Study, Seoul), Philip Lu (Korea Inst. Advanced Study, Seoul)</author>
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<title>(Quasi-)normal modes of rotating black holes and new solitons in Einstein-Gauss-Bonnet</title>
<description><span>In this paper, we analyze the scalar field (quasi-)normal modes of recently derived rotating black holes within the framework of Einstein-Gauss-Bonnet theory at the Chern-Simons point in five dimensions. We also examine the mode spectrum of these probes on new static gravitational solitons. These solitons, featuring a regular center, are constructed from static black holes with gravitational hair via a double analytic continuation. By imposing ingoing boundary conditions at the horizons of rotating black holes, ensuring regularity at the soliton centers, and imposing Dirichlet boundary conditions at infinity, we obtain numerical spectra for the rotating black holes and solitons. For static black holes, we demonstrate analytically that the imaginary part of the mode frequencies is negative. Our analysis of the massless Klein-Gordon equation on five-dimensional geometries reveals an infinite family of gapped, massive three-dimensional Klein-Gordon fields, despite the presence of a non-compact extended direction. For the static solitons, the frequencies are real and non-equispaced, whereas in the rotating black holes, counter-rotating modes are absorbed more quickly, and the imaginary part of the co-rotating modes approaches zero as extremality is approached. Additionally, we show that both the rotating black holes and solitons can be equipped with non-trivial torsion, leading to a novel branch of solutions.</span></description>
<link>https://inspirehep.net/literature/2847468</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847468</guid>
<pubDate>Wed, 13 Nov 2024 04:23:31 GMT</pubDate>
<author>Lilianne Tapia (Concepcion U.), Monserrat Aguayo (Concepcion U.), Andrés Anabalón (Concepcion U.), Dumitru Astefanesei (Valparaiso U., Catolica), Nicolás Grandi (UNLP, La Plata (main), La Plata U.), Fernando Izaurieta (Unlisted, CL, San Sebastian U., Chile), Julio Oliva (Concepcion U.), Cristian Quinzacara (Unlisted, CL, San Sebastian U., Chile)</author>
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<title>Power spectrum of scalar fluctuations of the metric during the formation of a scalar black hole in inflation</title>
<description><span>In this paper we use the collapse metric obtained by Carneiro and Fabris to calculate the power spectrum associated to gauge invariant fluctuations of the metric during the formation of a primordial scalar black hole at the end of inflation. We assume that local perturbations in the vacuum energy density can collapse by means of the collapse of the local inflaton field, generating a singularity as shown by Carneiro and Fabris. Employing a representative term of the series expansion of the scale factor we obtain a nearly scale invariant power spectrum for a second order approximation of the scale factor. Thus, the spectrum for scalar black holes obtained can be considered as a correction of the power spectrum of the primordial quantum fluctuations of the inflaton field.</span></description>
<link>https://inspirehep.net/literature/2847464</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847464</guid>
<pubDate>Wed, 13 Nov 2024 04:23:10 GMT</pubDate>
<author>José Edgar Madriz Aguilar (Guadalajara U., Unlisted, MX), J.O. Valle (Guadalajara U.), M. Montes (Paraiba U.), C. Romero</author>
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<title>The stability of the greybody factor of Hayward black hole</title>
<description><span>In this study, we investigate the stability of the greybody factor of Hayward black holes by adding a small bump to the effective potential. Considering the greybody factor is a function of frequency, we define the so-called $\mathcal{G}$-factor and $\mathcal{H}$-factor to quantitatively characterize its stability. We study the stability of the greybody factor within the equal amplitude method and the equal energy method, respectively. Here, the equal amplitude method can be directly imposed by fixing the amplitude of the bump, while the equal energy method requires a physical definition of the energy of the bump with the assistance of hyperboloidal framework. For both the equal amplitude method and the equal energy method, when the location of the bump is close to the event horizon of the black hole, and the closer it is to the peak of original potential, the larger are $\mathcal{G}$-factor and $\mathcal{H}$-factor, and they are bounded by the magnitude of the amplitude or the energy. More importantly, for the equal amplitude method, two factors tend to a specific value as the location of the bump increases. In contrast, for the equal energy method, two factors converge to zero as the location of the bump increases. Notably, the $\mathcal{G}$-factor and the $\mathcal{H}$-factor are insensitive to the regular parameter of Hayward black hole. Therefore, our results indicate that the greybody factor is stable under specific perturbations.</span></description>
<link>https://inspirehep.net/literature/2847455</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847455</guid>
<pubDate>Wed, 13 Nov 2024 04:23:00 GMT</pubDate>
<author>Liang-Bi Wu (HIAS, UCAS, Hangzhou, Beijing, Inst. High Energy Phys., Beijing, GUCAS), Rong-Gen Cai (HIAS, UCAS, Hangzhou, Beijing, Inst. Theor. Phys., Ningbo U.), Libo Xie (HIAS, UCAS, Hangzhou, Beijing, Inst. Theor. Phys., Beijing, Inst. High Energy Phys., Beijing, GUCAS)</author>
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<title>Imprints of black hole charge on the precessing jet nozzle of M87*</title>
<description><span>The observed jet precession period of approximately 11 years for M87* strongly suggests the presence of a supermassive rotating black hole with a tilted accretion disk at the center of the galaxy. By modeling the motion of the tilted accretion disk particle with the spherical orbits around a Kerr-Newman black hole, we study the effect of charge on the observation of the precession period, thereby exploring the potential of this strong-gravity observation in constraining multiple black hole parameters. Firstly, we study the spherical orbits around a Kerr-Newman black hole and find that their precession periods increase with the charge. Secondly, we utilize the observed M87* jet precession period to constrain the relationship between the spin, charge, and warp radius, specifically detailing the correlations between each pair of these three quantities. Moreover, to further refine constraints on the charge, we explore the negative correlation between the maximum warp radius and charge. A significant result shows that the gap between the maximum warp radii of the prograde and retrograde orbits decrease with the black hole charge. If the warp radius is provided by other observations, different constraints on the charge can be derived for the prograde and retrograde cases. These results suggest that in the era of multi-messenger astronomy, such strong-gravity observation of precessing jet nozzle presents a promising avenue for constraining black hole parameters.</span></description>
<link>https://inspirehep.net/literature/2847454</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847454</guid>
<pubDate>Wed, 13 Nov 2024 04:22:55 GMT</pubDate>
<author>Xiang-Cheng Meng, Chao-Hui Wang, Shao-Wen Wei</author>
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<title>Primordial Black Hole Formation from Type II Fluctuations with Primordial Non-Gaussianity</title>
<description><span>This study investigates the formation of primordial black holes (PBHs) resulting from the collapse of adiabatic fluctuations with large amplitudes and non-Gaussianity. Ref. \cite{Uehara:2024yyp} showed that fluctuations with large amplitudes lead to the formation of type B PBHs, characterized by the existence of the bifurcating trapping horizons, distinct from the more common type A PBHs without a bifurcating trapping horizon. We focus on the local type non-Gaussianity characterized by the curvature perturbation $\zeta$ given by a function of a Gaussian random variable $\zeta_{\rm G}$ as $\beta\zeta=-\ln(1-\beta \zeta_{\rm G})$ with a parameter $\beta$. Then we examine how the non-Gaussianity influences the dynamics and the type of PBH formed, particularly focusing on type II fluctuations, where the areal radius varies non-monotonically with the coordinate radius. Our findings indicate that, for $\beta&gt;-2$, the threshold for distinguishing between type A and type B PBHs decreases with increasing $\beta$ similarly to the threshold for black hole formation. Additionally, for large positive values of $\beta$, the threshold for type B PBHs approaches that for type II fluctuations. We also find that, for a sufficiently large negative value of $\beta\lesssim-4.0$, the threshold value is in the type II region of $\mu$, i.e., there are fluctuations of type II that do not form black holes. Lastly, we calculate the PBH mass for several values of $\beta$. Then we observe that the final mass monotonically increases with the initial amplitude within the parameter region of type A PBHs, which differs from previous analytical expectations.</span></description>
<link>https://inspirehep.net/literature/2847452</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847452</guid>
<pubDate>Wed, 13 Nov 2024 04:22:51 GMT</pubDate>
<author>Masaaki Shimada (Nagoya U.), Albert Escrivá (Nagoya U.), Daiki Saito (Nagoya U.), Koichiro Uehara (Nagoya U.), Chul-Moon Yoo (Nagoya U.)</author>
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<title>Diving into a multi-band holographic superconductor</title>
<description><span>In this paper, we consider the interior structure of a multi-band holographic superconductor model. We focus on the holographic superconductor system with two scalar fields which correspond to two s-wave order parameters in the dual condensed matter system. With two s-wave order parameters, the boundary system has more interesting behaviors which can also be reflected in black hole interior structure. We find the Einstein-Rosen bridge collapse and Josephson oscillations of two scalar fields inside the horizon. For the region near the singularity, we find that the metric still presents Kasner form and there is also Kasner transition behavior. However, when two scalar fields coexist, the Kasner exponents and Kasner transition formula will be different from the single scalar field case. The different interior structures between multi-band holographic superconductor and single-band holographic superconductor we find in this work further confirms that the black hole interior is important to reflect the properties of dual condensed matter systems.</span></description>
<link>https://inspirehep.net/literature/2847453</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847453</guid>
<pubDate>Wed, 13 Nov 2024 04:22:48 GMT</pubDate>
<author>Xing-Kun Zhang (NUAA, Nanjing), Xin Zhao (NUAA, Nanjing), Zhang-Yu Nie (NUAA, Nanjing, Unlisted, CN), Ya-Peng Hu (NUAA, Nanjing), Yu-Sen An</author>
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<title>Quasinormal modes of Plebański-Demiański black hole in the near-Nariai regime</title>
<description><span>We investigates the massless scalar perturbations of the Plebański-Demiański black hole considering the general case that admits all nonzero parameters. This case is the most generic black hole spacetime in general relativity, characterized by mass, spin, acceleration, electric and magnetic charges, NUT parameter, and cosmological constant. Employing conformal transformations, we can separate the massless scalar field equation and reduce the effective potential in the radial perturbation equation into the Pöschl--Teller potential in the near-Nariai limit where the event and cosmo-acceleration horizons are close. This allows us to obtain an exact analytical solution of the quasinormal frequency, implying that the decay rate of the field is quantized depending only on the surface gravity of the black hole.</span></description>
<link>https://inspirehep.net/literature/2847451</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847451</guid>
<pubDate>Wed, 13 Nov 2024 04:22:32 GMT</pubDate>
<author>Hyewon Han (Dongguk U.), Bogeun Gwak (Dongguk U.)</author>
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<title>Nonlinear Effects in Black Hole Ringdown Made Simple: Quasi-Normal Modes as Adiabatic Modes</title>
<description><span>The nonlinear nature of general relativity manifests prominently throughout the merger of two black holes, from the inspiral phase to the final ringdown. Notably, the quasi-normal modes generated during the ringdown phase display significant nonlinearities. We show that these nonlinear effects can be effectively captured by zooming in on the photon ring through the Penrose limit. Specifically, we model the quasi-normal modes as null particles trapped in unstable circular orbits around the black holes and show that they can be interpreted as adiabatic modes, perturbations that are arbitrarily close to large diffeomorphisms. This enables the derivation of a simple analytical expression for the QNM nonlinearities for Schwarzschild and Kerr black holes which reproduces well the existing numerical results.</span></description>
<link>https://inspirehep.net/literature/2847447</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847447</guid>
<pubDate>Wed, 13 Nov 2024 04:22:16 GMT</pubDate>
<author>A. Kehagias (Natl. Tech. U., Athens, Geneva U., CAP), A. Riotto (Geneva U., CAP)</author>
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<title>Full 3D nonlinear dynamics of charged and magnetized boson stars</title>
<description><span>Gauged boson stars are exotic compact objects that can potentially mimic black holes or magnetized neutron stars in both their gravitational and electromagnetic signatures, offering a compelling new description or even an alternative explanation for various multimessenger phenomena. As a crucial step toward establishing boson stars as viable multimessenger sources, we perform 3D numerical simulations of the fully nonlinear Einstein-Maxwell-Klein-Gordon system, focusing on both spherical and axisymmetric boson star configurations that vary in their electromagnetic coupling between the neutral case up to values close to the critical case, and so their magnetic field content. For spherical configurations, we consistently find stable solutions. In contrast, for axially symmetric, electrically neutral, magnetized configurations, the dynamics are highly sensitive to the electromagnetic coupling. Configurations with stronger coupling develop a one-armed mode instability, which leads to collapse into black holes. Configurations with weaker coupling undergo a two-stage process: an initial bar-mode instability that triggers a one-armed spiral deformation. This eventually also results in black hole formation, accompanied by emissions of both gravitational and electromagnetic radiation. A similar instability and two-stage pattern is observed in all charged rotating boson stars analyzed. However, all of these configurations become stable when self-interactions are introduced.</span></description>
<link>https://inspirehep.net/literature/2847428</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847428</guid>
<pubDate>Wed, 13 Nov 2024 04:21:09 GMT</pubDate>
<author>Víctor Jaramillo (USTC, Hefei, CUST, SKLPDE), Darío Núñez (Mexico U., ICN, U. Aveiro (main)), Milton Ruiz (Valencia U., Astro. Astrophys.), Miguel Zilhão (U. Aveiro (main))</author>
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<title>Smooth extremal horizons are the exception, not the rule</title>
<description><span>We show that the general charged, rotating black hole in five-dimensional Einstein-Maxwell theory has a singular extremal limit. Only the known analytic solutions with exactly zero charge or zero angular momenta have smooth extremal horizons. When the two angular momenta are not equal and both are scaled to zero, the solution approaches a new family of static, nonspherical extremal black holes. We also consider general black holes in five-dimensional Einstein-Maxwell-Chern-Simons theory, and show that they also have singular extremal limits except for one special value of the coefficient of the Chern-Simons term (the one fixed by supergravity). Combining this with earlier results showing that extremal black holes have singular horizons in four-dimensional general relativity with small higher derivative corrections, and in anti-de Sitter space with perturbed boundary conditions, one sees that smooth extremal horizons are indeed the exception and not the rule.</span></description>
<link>https://inspirehep.net/literature/2847421</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847421</guid>
<pubDate>Wed, 13 Nov 2024 04:20:02 GMT</pubDate>
<author>Gary T. Horowitz (UC, Santa Barbara), Jorge E. Santos (Cambridge U., DAMTP)</author>
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<title>Subleading logarithmic behavior in the parquet formalism</title>
<description><span>The Fermi-edge singularity in x-ray absorption spectra of metals is a paradigmatic case of a logarithmically divergent perturbation series. Prior work has thoroughly analyzed the leading logarithmic terms. Here, we investigate the perturbation theory beyond leading logarithms and formulate self-consistent equations to incorporate all leading and next-to-leading logarithmic terms. This parquet solution of the Fermi-edge singularity goes beyond the previous first-order parquet solution and sheds new light on the parquet formalism regarding logarithmic behavior. We present numerical results in the Matsubara formalism and discuss the characteristic power laws. We also show that, within the single-boson exchange framework, multi-boson exchange diagrams are needed already at the leading logarithmic level.</span></description>
<link>https://inspirehep.net/literature/2847282</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847282</guid>
<pubDate>Tue, 12 Nov 2024 06:45:39 GMT</pubDate>
<author>Marcel Gievers, Richard Schmidt, Jan von Delft, Fabian B. Kugler</author>
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<title>A Systematic Search for Candidate Supermassive Black Hole Binaries Using Periodic Mid-Infrared Light Curves of Active Galactic Nuclei</title>
<description><span>Periodic variability in active galactic nuclei (AGNs) is a promising method for studying sub-parsec supermassive black hole binaries (SMBHBs), which are a challenging detection target. While extensive searches have been made in the optical, X-ray and gamma-ray bands, systematic infrared (IR) studies remain limited. Using data from the Wide-field Infrared Survey Explorer (WISE), which provides unique decade-long mid-IR light curves with a six-month cadence, we have conducted the first systematic search for SMBHB candidates based on IR periodicity. Analyzing a parent sample of 48,932 objects selected from about half a million AGNs, we have identified 28 candidate periodic AGNs with periods ranging from 1,268 to 2,437 days (in the observer frame) by fitting their WISE light curves with sinusoidal functions. However, our mock simulation of the parent sample indicates that stochastic variability can actually produce a similar number of periodic sources, underscoring the difficulty in robustly identifying real periodic signals with WISE light curves, given their current sampling. Notably, we found no overlap between our sample and optical periodic sources, which can be explained by a distinct preference for certain periods due to selection bias. By combining archived data from different surveys, we have identified SDSS J140336.43+174136.1 as a candidate exhibiting periodic behavior in both optical and IR bands, a phenomenon that warrants further validation through observational tests. Our results highlight the potential of IR time-domain surveys, including future missions such as the Nancy Grace-Roman Space Telescope, for identifying periodic AGNs, but complementary tests are still needed to determine their physical origins such as SMBHBs.</span></description>
<link>https://inspirehep.net/literature/2847214</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847214</guid>
<pubDate>Tue, 12 Nov 2024 04:35:24 GMT</pubDate>
<author>Di Luo, Ning Jiang, Xin Liu</author>
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<title>Analytically Exact Quantum Simulation of N-Body Interactions via Untunable Decentralized Hamiltonians for Implementing the Toric Code and Its Modifica...</title>
<description><span>We propose a new quantum simulation method for simulating N-body interactions, which are tensor products of N Pauli operators, in an analytically exact manner. This method iteratively attaches many two-body interactions on one two-body interaction to simulate an N-body interaction. Those controlled two-body interactions can be untunable and act only on neighboring spins. The strength difference between controlled and target Hamiltonians is normally not more than one order of magnitude. This simulation is theoretically error-free, and errors due to experimental imperfections are ignorable. A major obstacle to simulating the toric code model and modified toric codes used in topological quantum computation is to simulate N-body interactions. We employ the new quantum simulation method to solve this issue and thus simulate the toric code model and its modifications.</span></description>
<link>https://inspirehep.net/literature/2847215</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847215</guid>
<pubDate>Tue, 12 Nov 2024 04:35:08 GMT</pubDate>
<author>Haochen Zhao (Imperial Coll., London), Florian Mintert (Imperial Coll., London, HZDR, Dresden)</author>
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<title>Thermodynamics of Einstein-Gauss-Bonnet Black Holes and Ensemble-averaged Theory</title>
<description><span>In this paper, using the ensemble-averaged theory, we define the thermodynamic free energy of Einstein-Gauss-Bonnet (EGB) black holes in anti-de Sitter (AdS) spacetime. This approach derives the gravitational partition function by incorporating non-saddle geometries besides the classical solutions. Unlike the sharp transition points seen in free energy calculated via saddle-point approximation, the ensemble-averaged free energy plotted against temperature shows a smoother behavior, suggesting that black hole phase transitions may be viewed as a small $G_N$ (Newton's gravitational constant) limit of the ensemble theory. This is similar to the behavior of black hole solutions in Einstein's gravity theory in AdS spacetime. We have obtained an expression for the quantum-corrected free energy for EGB-AdS black holes, and in the six-dimensional case, we observe a well-defined local minimum after the transition temperature which was absent in the earlier analysis of the classical free energy landscape. Furthermore, we expand the ensemble-averaged free energy in powers of $G_N$ to identify non-classical contributions. Our findings indicate that the similarities in the thermodynamic behavior between five-dimensional EGB-AdS and Reissner-Nordström-AdS (RN-AdS) black holes, as well as between six-dimensional EGB-AdS and Schwarzschild-AdS black holes, extend beyond the classical regime.</span></description>
<link>https://inspirehep.net/literature/2847120</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847120</guid>
<pubDate>Tue, 12 Nov 2024 04:23:44 GMT</pubDate>
<author>Md Sabir Ali (APC Roy Gov. Coll.), C. Fairoos (TKM Coll. Arts Sci.), C.L. Ahmed Rizwan (Payyanur Coll.), T.K. Safir (TKM Coll. Arts Sci.), Peng Cheng (Tianjin U.)</author>
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<title>Particle creation and evaporation in Kalb-Ramond gravity</title>
<description><span>In this work, we examine particle creation and the evaporation process in the context of Kalb-Ramond gravity. Specifically, we build upon two existing solutions from the literature \cite{yang2023static} and \cite{Liu:2024oas}, both addressing a static, spherically symmetric configuration. For this study, we focus on the scenario in which the cosmological constant vanishes. To begin, the corrections to Hawking radiation for bosonic modes are examined by studying the Klein-Gordon equation in curved spacetime. Through the calculation of Bogoliubov coefficients, we identify how the parameter $\ell$, which governs Lorentz symmetry breaking, contributes a correction to the amplitude associated with particle production. Within this approach, the power spectrum and Hawking temperature are derived. Additionally, we obtain expressions for the power spectrum and particle number density by analyzing Hawking radiation from a tunneling viewpoint. A parallel approach is applied to fermionic modes. Finally, we examine black hole evaporation, finding that the black hole lifetime in these cases can be determined analytically.</span></description>
<link>https://inspirehep.net/literature/2847118</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847118</guid>
<pubDate>Tue, 12 Nov 2024 04:23:03 GMT</pubDate>
<author>A.A. Araújo Filho (Paraiba U.)</author>
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<item>
<title>Optical Properties, Quasinormal Modes and Greybody factors of deformed AdS-Schwarzschild black holes</title>
<description><span>We investigate the temperature, photon and shadow radii, quasinormal modes (QNMs), greybody factors, and emission rates of deformed AdS black holes, focusing on the effects of the deformation parameter $ \alpha $ and control parameter $ \beta $. Increasing $ \alpha $ enhances the oscillation frequency and damping rate of gravitational waves, while $ \beta $ shows non-linear behaviour. Electromagnetic perturbations exhibit similar trends, though with lower frequencies and damping rates. Greybody factors are mainly influenced by multipole moment $ l $ and $ \alpha $, with $ \beta $ having a more subtle effect. These findings provide insights into black hole dynamics, mergers, and gravitational wave emissions.</span></description>
<link>https://inspirehep.net/literature/2847115</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847115</guid>
<pubDate>Tue, 12 Nov 2024 04:22:56 GMT</pubDate>
<author>Dhruba Jyoti Gogoi (Unlisted, IN, SISSA, Trieste, ICTP, Trieste, Dibrugarh U.), Jyatsnasree Bora (Dibrugarh U.), Filip Studnička (Hradec Kralove U.), H. Hassanabadi (Hradec Kralove U.)</author>
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<item>
<title>Inferring jet physics from neutron star - black hole mergers with gravitational waves</title>
<description><span>Neutron star - black hole (NSBH) mergers that undergo tidal disruption may launch jets that could power a gamma-ray burst. We use a population of simulated NSBH systems to measure jet parameters from the gravitational waves emitted by these systems. The conditions during the tidal disruption and merger phase required to power a gamma-ray burst are uncertain. It is likely that the system must achieve some minimum remnant baryonic mass after the merger before a jet can be launched to power a gamma-ray burst. Assuming a fiducial neutron star equation of state, we show how Bayesian hierarchical inference can be used to infer the minimum remnant mass required to launch a gamma-ray burst jet as well as the maximum gamma-ray burst viewing angle to detect a gamma-ray burst. We find that with 200 NSBH observations, we can measure the minimum disk mass to within 0.01 solar masses at 90% credibility. We simultaneously infer the maximum gamma-ray burst viewing angle to within 13 degrees at 90% credibility. We conclude that upcoming upgrades to the LIGO observatories may provide important new insights into the physics of NSBH jets.</span></description>
<link>https://inspirehep.net/literature/2847106</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847106</guid>
<pubDate>Tue, 12 Nov 2024 04:22:13 GMT</pubDate>
<author>Teagan A. Clarke, Paul D. Lasky, Eric Thrane</author>
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<item>
<title>Gravity and fluid dynamic correspondence on a null hypersurface: inconsistencies and advancement</title>
<description><span>Unlike black hole thermodynamics, the fluid-gravity correspondence of a generic null surface appears to be ``incomplete''; though both approaches point to the emergent nature of gravitation. In the existing formulation of fluid-gravity correspondence of a null surface, we have only the momentum conservation relation in the form of the Damour-Navier-Stokes (DNS) equation. The other relations, such as the energy conservation relation, continuity relation, etc., are almost non-existent and are discussed sporadically in literature for stretched horizons. Furthermore, the fluid-gravity correspondence is not formulated from a suitable energy-momentum tensor in the conventional manner. In the paper, we address these issues. By giving the energy conservation relation, we improve the fluid-gravity analogy on a generic null hypersurface. Additionally, by introducing a suitable energy-momentum tensor, which forms the basis of the entire fluid description, we formulate the entire fluid description of the null surface. Moreover, we provide the expression of continuity relation in the context of fluid-gravity correspondence. The entire analysis has been done for a generic null surface, which differs from the existing stretched horizon approach and, thereby, expands the scope of applicability for any arbitrary null surface.</span></description>
<link>https://inspirehep.net/literature/2847096</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847096</guid>
<pubDate>Tue, 12 Nov 2024 04:21:34 GMT</pubDate>
<author>Krishnakanta Bhattacharya (IUCAA, Pune), Sumit Dey (Warsaw U.), Bibhas Ranjan Majhi (Indian Inst. Tech., Guwahati)</author>
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<item>
<title>Premerger observation and characterization of massive black hole binaries</title>
<description><span>We demonstrate an end-to-end technique for observing and characterizing massive black hole binary signals before they merge with the LISA space-based gravitational-wave observatory. Our method uses a zero-latency whitening filter, originally designed for rapidly observing compact binary mergers in ground-based observatories, to be able to observe signals with no additional latency due to filter length. We show that with minimal computational cost, we are able to reliably observe signals as early as 14 days premerger as long as the signal has accrued a signal-to-noise ratio of at least 8 in the LISA data. We also demonstrate that this method can be used to characterize the source properties, providing early estimates of the source's merger time, chirp mass, and sky localization. Early observation and characterization of massive black holes is crucial to enable the possibility of rapid multimessenger observations, and to ensure that LISA can enter a protected operating period when the merger signal arrives.</span></description>
<link>https://inspirehep.net/literature/2847029</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2847029</guid>
<pubDate>Tue, 12 Nov 2024 04:15:08 GMT</pubDate>
<author>Gareth Cabourn Davies (Portsmouth U., ICG), Ian Harry (Portsmouth U., ICG), Michael J. Williams (Portsmouth U., ICG), Diganta Bandopadhyay (Birmingham U.), Leor Barack (Southampton U.), Jean-Baptiste Bayle (SUPA, UK, Glasgow U.), Charlie Hoy (Portsmouth U., ICG), Antoine Klein (Birmingham U.), Hannah Middleton (Birmingham U.), Christopher J. Moore (Birmingham U.), Laura Nuttall (Portsmouth U., ICG), Geraint Pratten (Birmingham U.), Alberto Vecchio (Birmingham U.), Graham Woan (SUPA, UK, Glasgow U.)</author>
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<title>Causality, extremality, and all that</title>
<description><span>It is well known that general relativity, when viewed from the perspective of quantum field theory, is a non-renormalisable theory --- this is central to the problem of quantum gravity. A less problematic perspective is to view general relativity from the perspective of effective field theory. As such, the Einstein-Hilbert action is considered just the lowest-order term in a derivative expansion, where higher-order terms are suppressed and agnostically parameterise the effects of an unknown UV completion. It was thought that all effective actions of this form are able to accurately capture the effect of UV physics at low energies, but certain observables within the low-energy theories can tip us off about possibly undesirable properties of UV completions. In this thesis, we are concerned with such qualitative features of low-energy gravitational effective field theories. In the first part, we will consider the restrictions that causality puts on the Wilson coefficients of an effective field theory. To that end, we first establish the use of an appropriate notion of causality and find consistency with gravitational positivity bounds. We then apply this so-called infrared causality to put constraints on the leading-order EFT of gravity on black hole and pp-wave backgrounds in five or higher dimensions. In the second part, we are concerned with qualitative features of extremal black holes, the kinematics of which are known to have interesting implications on quantum gravity. We first study deformations to the near-horizon region of known extremal black holes and use intuition from these to state a conjecture on Wilson coefficients in terms of the behaviour of the deformations near the horizon. Finally, we consider a prototypical scalar field toy example for restrictions on EFTs in the context of $\mathrm{AdS}_{2}$ holography.</span></description>
<link>https://inspirehep.net/literature/2846967</link>
<guid isPermaLink="false">https://inspirehep.net/literature/2846967</guid>
<pubDate>Mon, 11 Nov 2024 18:16:40 GMT</pubDate>
<author>Calvin Yi-Ren Chen (Imperial Coll., London)</author>
</item>
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