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DTSTART;TZID=America/New_York:20231205T110000
DTEND;TZID=America/New_York:20231205T120000
DTSTAMP:20260404T232950
CREATED:20240226T112803Z
LAST-MODIFIED:20240813T160712Z
UID:10002870-1701774000-1701777600@cmsa.fas.harvard.edu
SUMMARY:The Feynman propagator and self-adjointness
DESCRIPTION:General Relativity Seminar \nSpeaker: Andras Vasy (Stanford) \nTitle: The Feynman propagator and self-adjointness \nAbstract: In this talk I will discuss the Feynman and anti-Feynman inverses for wave operators on certain Lorentzian manifolds; these are two inverses which from a microlocal analysis perspective are more natural than the standard causal (advanced/retarded) ones. For instance\, for the spectral family of the wave operator\, these are the natural inverses when the spectral parameter is non-real. Indeed\, I will explain that these connect to the self-adjointness of the wave operator\, and the positivity properties that follow. \n 
URL:https://cmsa.fas.harvard.edu/event/gr_12523/
LOCATION:Virtual
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-12.05.2023.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20231128T110000
DTEND;TZID=America/New_York:20231128T120000
DTSTAMP:20260404T232950
CREATED:20240223T051146Z
LAST-MODIFIED:20240223T051146Z
UID:10002813-1701169200-1701172800@cmsa.fas.harvard.edu
SUMMARY:Remarkable symmetries of rotating black holes
DESCRIPTION:General Relativity Seminar \nSpeaker: David Kubiznak (Charles University) \nTitle: Remarkable symmetries of rotating black holes \nAbstract: It is well known that the Kerr geometry admits a non-trivial Killing tensor and its ‘square root’ known as the Killing-Yano tensor. These two objects stand behind Carter’s constant of geodesic motion as well as allow for separability of test field equations in this background. The situation is even more remarkable in higher dimensions\, where a single object — the principal Killing-Yano tensor — generates a tower of explicit and hidden symmetries responsible for integrability of geodesics and separability of test fields around higher-dimensional rotating black holes. Interestingly\, similar yet different structure is already present for the slowly rotating black holes described by the `magic square’ version of the Lense-Thirring solution\, giving rise to a geometrically preferred spacetime that can be cast in the Painleve-Gullstrand form and admits a tower of exact rank-2 and higher rank Killing tensors whose number rapidly grows with the number of spacetime dimensions.
URL:https://cmsa.fas.harvard.edu/event/gr_112823/
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-11.28.23_Page_1.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20231114T110000
DTEND;TZID=America/New_York:20231114T120000
DTSTAMP:20260404T232950
CREATED:20240223T052212Z
LAST-MODIFIED:20240223T052212Z
UID:10002814-1699959600-1699963200@cmsa.fas.harvard.edu
SUMMARY:Quasi-Local Mass in a Binary Black Hole Merger
DESCRIPTION:General Relativity Seminar \nSpeaker: Daniel Kolb (Max Planck Institute) \nTitle: Quasi-Local Mass in a Binary Black Hole Merger \nAbstract: One of the major open problems in classical general relativity is how one should define the mass of a finite region of space. In this talk\, we will investigate a promising definition proposed by Wang and Yau in 2009. A closed 2-surface bounding the region of interest is embedded isometrically into Minkowski space. The mass is then calculated by comparing the extrinsic geometries. The Wang-Yau mass has many desirable properties\, but it has previously not been calculated for surfaces in dynamical spacetimes. To remedy this\, we will discuss how the Wang-Yau mass can be computed in practice and extend the definition to surfaces important in black hole dynamics: their quasi-local horizons. Finally\, we look at how this mass behaves in a merger of black holes.
URL:https://cmsa.fas.harvard.edu/event/gr_111423/
LOCATION:Virtual
CATEGORIES:General Relativity Seminar
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20231107T110000
DTEND;TZID=America/New_York:20231107T120000
DTSTAMP:20260404T232950
CREATED:20240223T052707Z
LAST-MODIFIED:20240223T052707Z
UID:10002816-1699354800-1699358400@cmsa.fas.harvard.edu
SUMMARY:Fluid stabilization in slowly expanding cosmological spacetime
DESCRIPTION:General Relativity Seminar \nSpeaker: David Fajman (Vienna) \nTitle: Fluid stabilization in slowly expanding cosmological spacetime \nAbstract: Relativistic fluids are known to form shocks during their evolution from near-homogeneous initial data. In expanding spacetimes\, shock formation is suppressed\, if the expansion is sufficiently strong. We refer to this effect as fluid stabilization. The occurrence of this phenomenon depends on features of the fluid and has implications for our understanding of structure formation and cosmological evolution. While the effect is well studied in the regime of accelerated expansion\, in recent years it has been shown that fluid stabilization occurs as well in spacetimes with slower expansion rates. In this talk we present different recent results on fluid stabilization in slowly expanding spacetimes and aspects of the methods involved in the respective proofs. \n  \nTalk via Zoom\, broadcast in G10 \n 
URL:https://cmsa.fas.harvard.edu/event/gr_11723/
LOCATION:Hybrid – G10
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-11.07.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20231024T110000
DTEND;TZID=America/New_York:20231024T120000
DTSTAMP:20260404T232950
CREATED:20240223T053357Z
LAST-MODIFIED:20240223T053357Z
UID:10002817-1698145200-1698148800@cmsa.fas.harvard.edu
SUMMARY:Resolving memory in numerical relativity\, and fixing BMS frames for modeling
DESCRIPTION:General Relativity Seminar \nSpeaker: Leo Stein (Mississippi) \nTitle: Resolving memory in numerical relativity\, and fixing BMS frames for modeling \nAbstract: Numerical relativity waveforms serve as ground truth for detection and parameter estimation of binary black hole mergers. Most NR waveforms to date miss memory effects\, as they were extracted from simulations using an approximation called extrapolation. I will report on the SXS collaboration’s capacity to resolve memory effects in production NR simulations using Cauchy-characteristic evolution (CCE)\, and in the future with Cauchy-characteristic matching (CCM). I will further report on how BH perturbation and post-Newtonian theory furnish natural BMS frames. With these BMS frames\, we can extract well-defined remnant quantities\, perform precision ringdown modeling\, and build complete surrogate waveform models that capture memory effects.
URL:https://cmsa.fas.harvard.edu/event/gr_102423/
CATEGORIES:General Relativity Seminar
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20231010T110000
DTEND;TZID=America/New_York:20231010T120000
DTSTAMP:20260404T232950
CREATED:20240223T054233Z
LAST-MODIFIED:20240223T054233Z
UID:10002819-1696935600-1696939200@cmsa.fas.harvard.edu
SUMMARY:Tidal Squeezing of Black Holes
DESCRIPTION:General Relativity Seminar \nSpeaker: Maria Rodriguez (Utah) \nTitle: Tidal Squeezing of Black Holes \nAbstract: Recent developments indicate that Kerr black holes do not deform when perturbed by a static external gravitational field. Relying on hidden symmetries\, compelling progress has been achieved to explain that Love numbers for Kerr black holes vanish. How does the phenomenon of tidal squeezing manifest in broader contexts? An elementary presentation of dynamical tidal squeezing of Kerr black holes will be given.
URL:https://cmsa.fas.harvard.edu/event/gr_101023/
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-10.10.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20231003T110000
DTEND;TZID=America/New_York:20231003T120000
DTSTAMP:20260404T232950
CREATED:20240223T054715Z
LAST-MODIFIED:20240223T054715Z
UID:10002820-1696330800-1696334400@cmsa.fas.harvard.edu
SUMMARY:A Smooth Horizon without a Smooth Horizon
DESCRIPTION:General Relativity Seminar \nSpeaker: Chethan Krishnan (IISc Bangalore) \nTitle: A Smooth Horizon without a Smooth Horizon \nAbstract: I will talk about some work that is about to appear\, where we note one precise way in which the stretched horizon can simulate a smooth horizon. I will also make an effort to put things in some perspective (brickwalls\, fuzzballs\, Type I algebras\,…)
URL:https://cmsa.fas.harvard.edu/event/gr_10323/
CATEGORIES:General Relativity Seminar
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230919T110000
DTEND;TZID=America/New_York:20230919T120000
DTSTAMP:20260404T232950
CREATED:20240223T101246Z
LAST-MODIFIED:20240223T101246Z
UID:10002846-1695121200-1695124800@cmsa.fas.harvard.edu
SUMMARY:Quantization of causal diamonds in 2+1 dimensional gravity
DESCRIPTION:General Relativity Seminar \nSpeaker: Rodrigo Silva\, University of Maryland \nTitle: Quantization of causal diamonds in 2+1 dimensional gravity \nAbstract: We develop the reduced phase space quantization of causal diamonds in $2+1$ dimensional gravity with a nonpositive cosmological constant. The system is defined as the domain of dependence of a spacelike topological disk with a fixed boundary metric. By solving the constraints in a constant-mean-curvature time gauge and removing all the spatial gauge redundancy\, we find that the phase space is the cotangent bundle of $Diff^+(S^1)/PSL(2\, \mathbb{R})$\, i.e.\, the group of orientation-preserving diffeomorphisms of the circle modulo the projective special linear subgroup. Classically\, the states correspond to causal diamonds embedded in $AdS_3$ (or $Mink_3$ if $\Lambda = 0$)\, with a fixed corner length\, that has the topological disk as a Cauchy surface. Because this phase space does not admit a global system of coordinates\, a generalization of the standard canonical (coordinate) quantization is required — in particular\, since the configuration space is a homogeneous space for a Lie group\, we apply Isham’s group-theoretic quantization scheme. The Hilbert space of the associated quantum theory carries an irreducible unitary representation of the $BMS_3$ group and can be realized by wavefunctions on a coadjoint orbit of Virasoro with labels in irreducible unitary representations of the corresponding little group. A surprising result is that the twist of the diamond boundary loop is quantized in terms of the ratio of the Planck length to the corner length. \n 
URL:https://cmsa.fas.harvard.edu/event/gr_91923/
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-09.19.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230912T110000
DTEND;TZID=America/New_York:20230912T120000
DTSTAMP:20260404T232950
CREATED:20240223T102522Z
LAST-MODIFIED:20240223T102522Z
UID:10002847-1694516400-1694520000@cmsa.fas.harvard.edu
SUMMARY:Pole skipping\, quasinormal modes\, shockwaves and their connection to chaos
DESCRIPTION:General Relativity Seminar \nSpeaker: Diandian Wang(Harvard University) \nTitle: Pole skipping\, quasinormal modes\, shockwaves and their connection to chaos \nAbstract: A chaotic quantum system can be studied using the out-of-time-order correlator (OTOC). I will tell you about pole skipping — a recently discovered feature of the retarded Green’s function — that seems to also know things: things like the Lyapunov exponent and the butterfly velocity\, which are important quantifiers of the OTOC. Then I will talk about a systematic way of deriving pole-skipping conditions for general holographic CFTs dual to classical bulk theories and how to use this framework to derive a few interesting statements including: (1) theories with higher spins generally violate the chaos bound; (2) the butterfly velocity calculated using pole skipping agrees with that calculated using shockwaves for arbitrary higher-derivative gravity coupled to ordinary matter; (3) shockwaves are related to a special type of quasinormal modes. As we will see\, the techniques are entirely classically gravitational\, which I will go through with a certain level of details.
URL:https://cmsa.fas.harvard.edu/event/gr_91223/
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-09.12.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230705T140000
DTEND;TZID=America/New_York:20230705T150000
DTSTAMP:20260404T232950
CREATED:20230818T045528Z
LAST-MODIFIED:20240215T112411Z
UID:10001127-1688565600-1688569200@cmsa.fas.harvard.edu
SUMMARY:Grey Galaxy’ as the endpoint of the Kerr-AdS super radiant blackhole
DESCRIPTION:General Relativity Seminar \nSpeaker: Suman Kundu (Weizmann Institute) \nTitle: ‘Grey Galaxy’ as the endpoint of the Kerr-AdS super radiant blackhole \nAbstract: Kerr AdS$_{d+1}$ black holes for $d\geq 3$ suffer from classical superradiant instabilities over a range of masses near extremality. We conjecture that these instabilities settle down into Grey Galaxies (GG)s – a new class of solutions to Einstein’s equations which we construct for $d=3$. Grey Galaxies consist of an $\omega=1$ black hole in the `centre’ of $AdS$\, surrounded by a uniformly thick and very large disk of thermal bulk matter that revolves around the centre of AdS at the speed of light. The parametrically low energy density and parametrically large radius of the gas disk are inversely related; as a consequence\, the gas carries a finite fraction of the total energy. Grey Galaxy saddles exist at masses that extend all the way down to the unitarity bound. Their thermodynamics is that of a weakly interacting mix of Kerr AdS black holes and the gas. In addition to a smooth piece\, the boundary stress tensor of these solutions includes a contribution from a delta function localized at the `equator’ of the boundary sphere\, a term which may be used as an order parameter that sharply distinguishes GG solutions from ordinary Kerr-Black hole saddles. We also construct `Revolving Black Hole (RBH) saddles’\,  macroscopically charged $SO(d\,2)$ descendants of AdS-Kerr solutions\, that describe black holes revolving around the centre of $AdS$\, at the fixed radial location but in a quantum wave function in the angular directions. RBH saddles turn out to be (marginally) entropically subdominant to GG saddles. We argue that supersymmetric versions of RBH saddles exist and have interesting consequences for the spectrum of SUSY states in\, e.g.  ${\cal N}=4$ Yang-Mills theory.
URL:https://cmsa.fas.harvard.edu/event/gr_7523/
LOCATION:Jefferson 453\, 17 Oxford St\, Cambridge\, MA 02138\, MA
CATEGORIES:General Relativity Seminar
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230511T133000
DTEND;TZID=America/New_York:20230511T143000
DTSTAMP:20260404T232950
CREATED:20230818T045112Z
LAST-MODIFIED:20240215T111322Z
UID:10001264-1683811800-1683815400@cmsa.fas.harvard.edu
SUMMARY:Positivity of Static quasi-local Mass in general relativity
DESCRIPTION:General Relativity Seminar \nSpeaker: Aghil Alaee\, Clark University \nTitle: Positivity of Static quasi-local Mass in general relativity \nAbstract: In this talk\, we review results on the PMT of quasi-local masses and prove the positivity of static quasi-local masses with respect to the AdS and AdS Schwarzschild spacetimes.
URL:https://cmsa.fas.harvard.edu/event/gr_51123/
LOCATION:Virtual
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-05.11.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230504T093000
DTEND;TZID=America/New_York:20230504T103000
DTSTAMP:20260404T232950
CREATED:20230818T044217Z
LAST-MODIFIED:20240228T073615Z
UID:10001263-1683192600-1683196200@cmsa.fas.harvard.edu
SUMMARY:Testing GR with GWs
DESCRIPTION:General Relativity Seminar \nSpeaker: Vitor Cardoso\, IST\, Lisbon and The Niels Bohr Institute\, Copenhagen \nTitle: Testing GR with GWs \nAbstract: One of the most remarkable possibilities of General Relativity concerns gravitational collapse to black holes\, leaving behind a geometry with light rings\, ergoregions and horizons. These peculiarities are responsible for uniqueness properties and energy extraction mechanisms that turn black holes into ideal laboratories of strong gravity\, of particle physics (yes!) and of possible quantum-gravity effects. I will discuss some of the latest progress in tests of General Relativity with black holes.
URL:https://cmsa.fas.harvard.edu/event/gr_5423/
LOCATION:CMSA Room G10\, CMSA\, 20 Garden Street\, Cambridge\, MA\, 02138\, United States
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-05.04.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230427T103000
DTEND;TZID=America/New_York:20230427T113000
DTSTAMP:20260404T232950
CREATED:20230818T043803Z
LAST-MODIFIED:20240119T052918Z
UID:10001262-1682591400-1682595000@cmsa.fas.harvard.edu
SUMMARY:The localized seed-to-solution method for the Einstein constraints
DESCRIPTION:General Relativity Seminar \nSpeaker: Philippe G. LeFloch\, Sorbonne University and CNRS \nTitle: The localized seed-to-solution method for the Einstein constraints \nAbstract: I will discuss advances on asymptotically Euclidian initial data sets and the variational method introduced by J. Corvino and R. Schoen. This talk is based on joint papers with The-Cang Nguyen (Montpellier) and Bruno Le Floch (Sorbonne Univ. and CNRS). In the vicinity of any given reference data set\, we define a “localized seed-to-solution” map\, which allows us to parametrize the initial data sets satisfying the Einstein constraints (possibly with matter fields). The parametrization is defined over classes of data sets understood modulo the image of the dual linearized constraints. Our main contribution concerns the sharp behavior of solutions at infinity\, which we can arbitrarily localize in asymptotic cones in the sense of A. Carlotto and R. Schoen. Most importantly\, as we prove it\, the solutions enjoy sharp decay estimates at the harmonic and super-harmonic levels. In the course of this analysis\, we discover the notion of ‘asymptotic modulators’\, as we call them\, or “correctors” to the standard ADM invariants.
URL:https://cmsa.fas.harvard.edu/event/gr_42723/
LOCATION:Virtual
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-04.27.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230424T133000
DTEND;TZID=America/New_York:20230424T143000
DTSTAMP:20260404T232950
CREATED:20230818T043218Z
LAST-MODIFIED:20240119T052608Z
UID:10001261-1682343000-1682346600@cmsa.fas.harvard.edu
SUMMARY:Recent advances in scalar curvature and positive mass theorems
DESCRIPTION:General Relativity Seminar \nSpeaker: Tin Yau Tsang\, University of California Irvine \nTitle: Recent advances in scalar curvature and positive mass theorems\n\nAbstract:  First\, we have a review of classical tools for studying scalar curvature and positive mass theorem. Then we are going to discuss some advances and new perspectives on these tools which lead to a deeper understanding of geometry and initial data sets.
URL:https://cmsa.fas.harvard.edu/event/gr_42423/
LOCATION:CMSA Room G10\, CMSA\, 20 Garden Street\, Cambridge\, MA\, 02138\, United States
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-04.24.23-1.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230413T093000
DTEND;TZID=America/New_York:20230413T103000
DTSTAMP:20260404T232950
CREATED:20230818T042744Z
LAST-MODIFIED:20240228T081413Z
UID:10001260-1681378200-1681381800@cmsa.fas.harvard.edu
SUMMARY:Resolving the photon ring
DESCRIPTION:General Relativity Seminar \nSpeaker: Shahar Hadar (University of Haifa) \nTitle: Resolving the photon ring \nAbstract: In the past few years\, the Event Horizon Telescope has released the first close-up interferometric images of two supermassive black holes\, M87* and SgrA*. It is believed that within these images is embedded a fine\, yet-unresolved brightness enhancement called the photon ring. The ring is a universal consequence of strong lensing by the black hole and thereby conveys information on its spacetime geometry\, potentially providing a new independent avenue for tests of general relativity in the strong-field regime. In the talk I will briefly review the theory of the photon ring and its corresponding spacetime region\, the photon shell\, which governs the universal lensing structure. I will then describe some current efforts and future prospects for resolving the ring\, which include both the construction of transformative new instruments and the development of novel analysis methods. Focusing on the latter\, I will present an upcoming proposal to use spectro-temporal autocorrelations in signals emitted from black hole environs as a probe of strong lensing effects.
URL:https://cmsa.fas.harvard.edu/event/gr_41323/
LOCATION:CMSA Room G10\, CMSA\, 20 Garden Street\, Cambridge\, MA\, 02138\, United States
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-04.13.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230406T093000
DTEND;TZID=America/New_York:20230406T103000
DTSTAMP:20260404T232950
CREATED:20230818T042449Z
LAST-MODIFIED:20240119T051939Z
UID:10001259-1680773400-1680777000@cmsa.fas.harvard.edu
SUMMARY:Rough solutions of the relativistic Euler equations
DESCRIPTION:General Relativity Seminar \nSpeaker: Sifan Yu\, Vanderbilt University \nTitle: Rough solutions of the relativistic Euler equations \nAbstract: I will discuss recent works on the relativistic Euler equations with dynamic vorticity and entropy. We use a new formulation of the equations\, which has geo-analytic structures. In this geometric formulation\, we decompose the flow into geometric “sound-wave part” and “transport-div-curl part”. This allows us to derive sharp results about the dynamics\, including the existence of low-regularity solutions. Then\, I will discuss the results of rough solutions of the relativistic Euler equations and the role that nonlinear geometric optics plays in the framework. Our main result is that the Sobolev norm $H^{2+}$ of the variables in the “wave-part” and the H\”older norm $C^{0\,0+}$ of the variables in the “transport-part” can be controlled in terms of initial data for short times. We note that the Sobolev norm assumption $H^{2+}$ is the optimal result for the variables in the “wave-part.” This talk will include the main ideas of the proof\, as well as a comparison of the relativistic and non-relativistic scenarios.
URL:https://cmsa.fas.harvard.edu/event/gr_4623/
LOCATION:CMSA Room G10\, CMSA\, 20 Garden Street\, Cambridge\, MA\, 02138\, United States
CATEGORIES:General Relativity Seminar
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230330T093000
DTEND;TZID=America/New_York:20230330T223000
DTSTAMP:20260404T232950
CREATED:20230818T042141Z
LAST-MODIFIED:20240118T101402Z
UID:10001258-1680168600-1680215400@cmsa.fas.harvard.edu
SUMMARY:Gravitational perturbations near to extreme Kerr
DESCRIPTION:General Relativity Seminar \nSpeaker: Alejandra Castro (University of Cambridge) \nTitle: Gravitational perturbations near to extreme Kerr \nAbstract: Gravitational perturbations of a black hole illustrate the invaluable synergy between theory\, experiment\, and numerical simulations in general relativity. A recent development in the theory side has been the identification of the relevant degrees of freedom describing the low energy physics driving a black hole away from extremality.  For simple cases\, this low energy sector determines important aspects of the gravitational backreaction\, and several properties that are key to our microscopic (quantum) understanding of black hole physics.\n\nIn this talk I will discuss these developments in the context of the (near-)extreme Kerr black hole. In particular\, I will revisit the spectrum of linear axisymmetric gravitational perturbations of this black hole. The aim is to characterise those perturbations that are responsible for the deviations away from extremality\, and to contrast them with the linearized perturbations treated in the Newman-Penrose formalism. I will show that for Kerr the low-lying mode sector is subtle and intricate—features that their charged spherical symmetric cousins do not display. This unveils new clues on how to decode a microscopic\, and holographic\, understanding of the Kerr black hole.
URL:https://cmsa.fas.harvard.edu/event/gr_33023/
LOCATION:CMSA Room G10\, CMSA\, 20 Garden Street\, Cambridge\, MA\, 02138\, United States
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-03.30.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230323T133000
DTEND;TZID=America/New_York:20230323T143000
DTSTAMP:20260404T232950
CREATED:20230818T041454Z
LAST-MODIFIED:20240118T100327Z
UID:10001257-1679578200-1679581800@cmsa.fas.harvard.edu
SUMMARY:New Phases of N=4 SYM
DESCRIPTION:General Relativity Seminar \nSpeaker: Prahar Mitra (University of Cambridge) \nTitle: New Phases of N=4 SYM \nAbstract: We construct new static solutions to gauged supergravity that\, via the AdS/CFT correspondence\, are dual to thermal phases in N=4 SYM at finite chemical potential. These solutions dominate the micro-canonical ensemble and are required to ultimately reproduce the microscopic entropy of AdS black holes. These are constructed in two distinct truncations of gauged supergravity and can be uplifted to solutions of type IIB supergravity. Together with the known phases of the truncation with three equal charges\, our findings permit a good understanding of the full phase space of SYM thermal states with three arbitrary chemical potentials. We will also discuss the status of hairy supersymmetric black hole solutions in this theory. \nBased on: https://arxiv.org/pdf/2207.07134.pdf [hep-th]
URL:https://cmsa.fas.harvard.edu/event/gr_32323/
LOCATION:CMSA Room G10\, CMSA\, 20 Garden Street\, Cambridge\, MA\, 02138\, United States
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-03.23.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230309T093000
DTEND;TZID=America/New_York:20230309T103000
DTSTAMP:20260404T232950
CREATED:20230817T185018Z
LAST-MODIFIED:20240228T091310Z
UID:10001256-1678354200-1678357800@cmsa.fas.harvard.edu
SUMMARY:Pseudospectrum and black hole quasinormal mode instability: An ultraviolet universality conjecture
DESCRIPTION:General Relativity Seminar \nSpeaker: Jose Luis Jaramillo (Bourgogne U.) \nTitle: Pseudospectrum and black hole quasinormal mode instability: an ultraviolet universality conjecture \nAbstract: Can we measure the ‘effective regularity’ of spacetime from the perturbation of quasi-normal mode (QNM) overtones? Black hole (BH) QNMs encode the resonant response of black holes under linear perturbations\, their associated complex frequencies providing an invariant probe into the background spacetime geometry. In the late nineties\, Nollert and Price found evidence of a BH QNM instability phenomenon\, according to which perturbed QNMs of Schwarzschild spacetime migrate to new perturbed branches of different qualitative behaviour and asymptotics. Here we revisit this BH QNM instability issue by adopting a pseudospectrum approach. Specifically\, we cast the QNM problem as an eigenvalue problem for a non-selfadjoint operator by adopting a hyperboloidal formulation of spacetime. Non-selfadjoint (more generally non-normal) operators suffer potentially of spectral instabilities\, the notion of pseudospectrum providing a tool suitable for their study. We find evidence that perturbed Nollert & Price BH QNMs track the pseudospectrum contour lines\, therefore probing the analytic structure of the resolvent\, showing the following (in)stability behaviour: i) the slowest decaying (fundamental) mode is stable\, whereas ii) (all) QNM overtones are ultraviolet unstable (for sufficiently high frequency). Building on recent work characterizing Burnett’s conjecture as a low-regularity problem in general relativity\, we conjecture that (in the infinite-frequency limit) generic ultraviolet spacetime perturbations make BH QNMs migrate to ‘Regge QNM branches’ with a precise universal logarithmic pattern. This is a classical general relativity (effective) low-regularity phenomenon\, agnostic to possible detailed (quantum) descriptions of gravity at higher-energies and potentially observationally accessible.
URL:https://cmsa.fas.harvard.edu/event/gr_3923/
LOCATION:CMSA Room G10\, CMSA\, 20 Garden Street\, Cambridge\, MA\, 02138\, United States
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-03.09.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230223T093000
DTEND;TZID=America/New_York:20230223T103000
DTSTAMP:20260404T232950
CREATED:20230817T184650Z
LAST-MODIFIED:20240118T093227Z
UID:10001255-1677144600-1677148200@cmsa.fas.harvard.edu
SUMMARY:Formation of trapped surfaces in the Einstein-Yang-Mills system
DESCRIPTION:General Relativity Seminar \nSpeaker: Nikolaos Athanasiou (University of Crete\, Greece) \nTitle: Formation of trapped surfaces in the Einstein-Yang-Mills system \nAbstract: The purpose of this talk is to give an overview of a semi-global existence result and a trapped surface formation results in the context of the Einstein-Yang-Mills system. Adopting a “signature for decay rates” approach first introduced by An\, we develop a novel gauge (and scale) invariant hierarchy of non-linear estimates for the Yang-Mills curvature which\, together with the estimates for the gravitational degrees of freedom\, yield the desired semi-global existence result. Once semi-global existence has been established\, we will explain how the formation of a trapped surface follows from a standard ODE argument. This is joint work with Puskar Mondal and Shing-Tung Yau.
URL:https://cmsa.fas.harvard.edu/event/gr_22323/
LOCATION:Virtual
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-02.23.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230216T133000
DTEND;TZID=America/New_York:20230216T143000
DTSTAMP:20260404T232950
CREATED:20230817T183826Z
LAST-MODIFIED:20240118T092821Z
UID:10001254-1676554200-1676557800@cmsa.fas.harvard.edu
SUMMARY:Quasinormal Modes from Penrose Limits
DESCRIPTION:General Relativity Seminar \nSpeaker: Kwinten Fransen (UC Santa Barbara) \nTitle: Quasinormal Modes from Penrose Limits \nAbstract: In this talk\, I will explain how to describe quasinormal modes with large real frequencies using Penrose limits. To do so\, I first recall relevant aspects of the Penrose limit\, and its resulting plane wave spacetimes\, as well as quasinormal modes to subsequently tie these together. Having established the main principle\, I will illustrate the usefulness of this point of view with the geometric realization of the emergent symmetry algebra underlying the quasinormal modes in the large real frequency limit and present its application to the astrophysically important example of Kerr black holes. Based on arXiv:2301.06999.
URL:https://cmsa.fas.harvard.edu/event/gr_21623/
LOCATION:CMSA Room G10\, CMSA\, 20 Garden Street\, Cambridge\, MA\, 02138\, United States
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-02.16.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230209T133000
DTEND;TZID=America/New_York:20230209T143000
DTSTAMP:20260404T232950
CREATED:20230817T183342Z
LAST-MODIFIED:20240215T100720Z
UID:10001253-1675949400-1675953000@cmsa.fas.harvard.edu
SUMMARY:Quasinormal modes and Ruelle resonances: mathematician's perspective
DESCRIPTION:General Relativity Seminar \nSpeaker: Maciej Zworski\, UC Berkeley \nTitle: Quasinormal modes and Ruelle resonances: mathematician’s perspective \nAbstract: Quasinormal modes of gravitational waves and Ruelle resonances in hyperbolic classical dynamics share many general properties and can be considered “scattering resonances”: they appear in expansions of correlations\, as poles of Green functions and are associated to trapping of trajectories (and are both notoriously hard to observe in nature\, unlike\, say\, quantum resonances in chemistry or scattering poles in acoustical scattering). I will present a mathematical perspective that also includes zeros of the Riemann zeta function (scattering resonances for the Hamiltonian given by the Laplacian on the modular surface) and stresses the importance of different kinds of trapping phenomena\, resulting\, for instance\, in fractal counting laws for resonances.
URL:https://cmsa.fas.harvard.edu/event/gr_2023/
LOCATION:CMSA Room G10\, CMSA\, 20 Garden Street\, Cambridge\, MA\, 02138\, United States
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-02.09.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230202T093000
DTEND;TZID=America/New_York:20230202T103000
DTSTAMP:20260404T232950
CREATED:20230817T182911Z
LAST-MODIFIED:20240118T092235Z
UID:10001252-1675330200-1675333800@cmsa.fas.harvard.edu
SUMMARY:Near extremal de Sitter black holes and JT gravity
DESCRIPTION:General Relativity Seminar \nSpeaker: Chiara Toldo (Harvard) \nTitle: Near extremal de Sitter black holes and JT gravity \nAbstract: In this talk I will explore the thermodynamic response near extremality of charged black holes in four-dimensional Einstein-Maxwell theory with a positive cosmological constant. The latter exhibit three different extremal limits\, dubbed cold\, Nariai and ultracold configurations\, with different near-horizon geometries. For each of these three cases I will analyze small deformations away from extremality\, and construct the effective two-dimensional theory\, obtained by dimensional reduction\, that captures these features. The ultracold case in particular shows an interesting interplay between the entropy variation and charge variation\, realizing a different symmetry breaking with respect to the other two near-extremal limits.
URL:https://cmsa.fas.harvard.edu/event/gr_2223/
LOCATION:Virtual
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-02.03.23.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20230126T093000
DTEND;TZID=America/New_York:20230126T103000
DTSTAMP:20260404T232950
CREATED:20230817T182501Z
LAST-MODIFIED:20240215T102816Z
UID:10001251-1674725400-1674729000@cmsa.fas.harvard.edu
SUMMARY:Testing spacetime geometry with images of supermassive compact objects: Current status and the future
DESCRIPTION:General Relativity Seminar \nSpeaker: Prashant Kocherlakota (BHI) \nTitle: Testing spacetime geometry with images of supermassive compact objects: Current status and the future \nAbstract: Astrophysical black holes (BHs) are expected to be described by the Kerr solution of the Einstein equations. Several frameworks have recently been developed to parametrically deform the Kerr metric in significantly different ways\, to enable formulations of tests of the no-hair theorems. Testing the viability status of alternative models – such as non-Kerr BHs from general relativity\, BHs from alternative theories\, wormholes\, and other exotic objects – as descriptors of astrophysical objects has been of longstanding interest. The Event Horizon Telescope (EHT) recently imaged Sagittarius A* (Sgr A*)\, the supermassive compact object at the center of the Galaxy\, making such tests possible. In such tests\, the shadow critical curve (or simply shadow boundary)\, defined on the observer’s image plane\, has gained prominence as the observable of interest. We will discuss how the EHT is able to extract information regarding the shadow of Sgr A* and the status of associated tests of the spacetime geometry in the strong-field regime. Future imaging measurements expect to detect the so-called photon ring\, a strong-gravitational lensing feature that appears in the close vicinity of the critical curve\, which houses higher-order images of the emission source. Time permitting\, we will also discuss how these can be used to set up more stringent tests of the spacetime metric and gravity in the future. \n\n 
URL:https://cmsa.fas.harvard.edu/event/gr_12623/
LOCATION:Virtual
CATEGORIES:General Relativity Seminar
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20221208T093000
DTEND;TZID=America/New_York:20221208T103000
DTSTAMP:20260404T232950
CREATED:20230817T182138Z
LAST-MODIFIED:20240228T111217Z
UID:10001250-1670491800-1670495400@cmsa.fas.harvard.edu
SUMMARY:A new proof for the nonlinear stability of slowly-rotating Kerr-de Sitter
DESCRIPTION:General Relativity Seminar \n\nSpeaker: Allen Fang (Princeton) \nTitle: A new proof for the nonlinear stability of slowly-rotating Kerr-de Sitter \nAbstract: The nonlinear stability of the slowly-rotating Kerr-de Sitter family was first proven by Hintz and Vasy in 2016 using microlocal techniques. In my talk\, I will present a novel proof of the nonlinear stability of slowly-rotating Kerr-de Sitter spacetimes that avoids frequency-space techniques outside of a neighborhood of the trapped set. The proof uses vector field techniques to uncover a spectral gap corresponding to exponential decay at the level of the linearized equation. The exponential decay of solutions to the linearized problem is then used in a bootstrap proof to conclude nonlinear stability.
URL:https://cmsa.fas.harvard.edu/event/gr_12822/
LOCATION:Virtual
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-12.08.22-1.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20221117T093000
DTEND;TZID=America/New_York:20221117T103000
DTSTAMP:20260404T232951
CREATED:20230817T181725Z
LAST-MODIFIED:20240118T090857Z
UID:10001249-1668677400-1668681000@cmsa.fas.harvard.edu
SUMMARY:Ringdown and geometry of trapping for black holes
DESCRIPTION:General Relativity Seminar \n\nSpeaker: Semyon Dyatlov (MIT) \nTitle: Ringdown and geometry of trapping for black holes \nAbstract: Quasi-normal modes are complex exponential frequencies appearing in long time expansions of solutions to linear wave equations on black hole backgrounds. They appear in particular during the ringdown phase of a black hole merger when the dynamics is expected to be driven by linear effects. In this talk I give an overview of various results in pure mathematics which relate asymptotic behavior of quasi-normal modes at high frequency to the geometry of the set of trapped null geodesics\, such as the photon sphere in Schwarzschild (-de Sitter). These trapped geodesics have two kinds of behavior: the geodesic flow is hyperbolic in directions normal to the trapped set (a feature stable under perturbations) and it is completely integrable on the trapped set. It turns out that normal hyperbolicity gives information about the rate of decay of quasi-normal modes\, while complete integrability gives rise to a quantization condition.
URL:https://cmsa.fas.harvard.edu/event/gr_111722/
LOCATION:Hybrid
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-11.17.22.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20221110T093000
DTEND;TZID=America/New_York:20221110T103000
DTSTAMP:20260404T232951
CREATED:20230817T181337Z
LAST-MODIFIED:20240118T090553Z
UID:10001248-1668072600-1668076200@cmsa.fas.harvard.edu
SUMMARY:Schwarzschild-like Topological Solitons in Gravity
DESCRIPTION:General Relativity Seminar \n\nSpeaker: Pierre Heidmann (Johns Hopkins) \nTitle: Schwarzschild-like Topological Solitons in Gravity \nAbstract: We present large classes of non-extremal solitons in gravity that are asymptotic to four-dimensional Minkowski spacetime plus extra compact dimensions. They correspond to smooth horizonless geometries induced by topology in spacetime and supported by electromagnetic flux\, which characterize coherent states of quantum gravity. We discuss a new approach to deal with Einstein-Maxwell equations in more than four dimensions\, such that they decompose into a set of Ernst equations. We generate the solitons by applying different techniques associated with the Ernst formalism. We focus on solitons with zero net charge yet supported by flux\, and compare them to Schwarzschild black holes. These are also ultra-compact geometries with very high redshift but differ in many aspects. At the end of the talk\, we discuss the stability properties of the solitons and their gravitational signatures.
URL:https://cmsa.fas.harvard.edu/event/gr_111022/
LOCATION:Virtual
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-11.10.22.png
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20221103T103000
DTEND;TZID=America/New_York:20221103T113000
DTSTAMP:20260404T232951
CREATED:20230817T180818Z
LAST-MODIFIED:20240209T063325Z
UID:10001247-1667471400-1667475000@cmsa.fas.harvard.edu
SUMMARY:Asymptotic geometry of null hypersurface in Schwarzschild spacetime and null Penrose inequality
DESCRIPTION:General Relativity Seminar \n\nSpeaker: Pengyu Le (BIMSA) \nTitle: Asymptotic geometry of null hypersurface in Schwarzschild spacetime and null Penrose inequality \nAbstract: Null Penrose inequality is an important case of the well-known Penrose inequality on a null hypersurface. It conjectures the relation between the area of the outmost marginally trapped surface and the Bondi mass at null infinity. Following the proposal of Christodoulou and Sauter\, we employ the perturbation method to study the asymptotic geometry of null hypersurfaces at null infinity in a perturbed vacuum Schwarzshild spacetime. We explain how to apply this perturbation theory to prove null Penrose inequality on a nearly spherically symmetric null hypersurface in a perturbed vacuum Schwarzschild spacetime.
URL:https://cmsa.fas.harvard.edu/event/gr_11322/
LOCATION:CMSA Room G10\, CMSA\, 20 Garden Street\, Cambridge\, MA\, 02138\, United States
CATEGORIES:General Relativity Seminar
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20221027T103000
DTEND;TZID=America/New_York:20221027T113000
DTSTAMP:20260404T232951
CREATED:20230817T180439Z
LAST-MODIFIED:20240118T090238Z
UID:10001246-1666866600-1666870200@cmsa.fas.harvard.edu
SUMMARY:Gravitational Wave\, Angular Momentum\, and Supertranslation Ambiguity
DESCRIPTION:General Relativity Seminar \n\nSpeaker: Naqing Xie (Fudan University) \nTitle: Gravitational Wave\, Angular Momentum\, and Supertranslation Ambiguity\n\nAbstract: The supertranslation ambiguity of angular momentum is a long-standing and conceptually important issue in general relativity. Recently\, there appeared the first definition of angular momentum at null infinity that is supertranslation invariant. However\, in the compact binary coalescence community\, supertranslation ambiguity is often ignored. We have shown that\, in the linearised theory of gravitational wave\, the new angular momentum coincides with the classical definition at the quadrupole level. This talk is based on a recent joint work with Xiaokai He and Xiaoning Wu.
URL:https://cmsa.fas.harvard.edu/event/gr_102722/
LOCATION:Virtual
CATEGORIES:General Relativity Seminar
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=America/New_York:20221020T103000
DTEND;TZID=America/New_York:20221020T113000
DTSTAMP:20260404T232951
CREATED:20240215T103645Z
LAST-MODIFIED:20240229T093550Z
UID:10002742-1666261800-1666265400@cmsa.fas.harvard.edu
SUMMARY:Love Symmetry of Black Holes
DESCRIPTION:General Relativity Seminar \nSpeaker: Sergei Dubovsky (New York University)\n\n\n\nTitle: Love Symmetry of Black Holes\n\n\nAbstract: Perturbations of massless fields in the Kerr-Newman black hole background enjoy a (“Love”) SL(2\,ℝ) symmetry in the suitably defined near zone approximation. We show how the intricate behavior of black hole responses in four and higher dimensions can be understood from the SL(2\,ℝ) representation theory. In particular\, static perturbations of four-dimensional black holes belong to highest weight SL(2\,ℝ) representations. It is this highest-weight property that forces the static Love numbers to vanish. We show that the Love symmetry is tightly connected to the enhanced isometries of extremal black holes. The Love symmetry also exhibits a peculiar UV/IR mixing.
URL:https://cmsa.fas.harvard.edu/event/gr_102022/
LOCATION:CMSA Room G10\, CMSA\, 20 Garden Street\, Cambridge\, MA\, 02138\, United States
CATEGORIES:General Relativity Seminar
ATTACH;FMTTYPE=image/png:https://cmsa.fas.harvard.edu/media/CMSA-GR-Seminar-10.20.22.png
END:VEVENT
END:VCALENDAR