Format results
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Talk
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Shape Dynamics: Perspectives and Problems
Julian Barbour University of Oxford
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The quantum equation of state of the universe produces a small cosmological constant
Tim Koslowski Technical University of Applied Sciences Würzburg-Schweinfurt
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Inflationary and pre-inflationary dynamics with the Starobinsky potential
Beatrice Bonga Radboud Universiteit Nijmegen
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Relationalism and the speed of light: Are we in a relationship?
Yuri Bonder Universidad Nacional Autónoma De Mexico (UNAM)
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Compact spherically symmetric solutions and gravitational collapse in SD
Flavio Mercati University of Naples Federico II
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Self-gravitating fluid solutions of Shape Dynamics
Daniel Guariento Conestoga College
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A Weyl-Type Theorem in Geometrized Newtonian Gravity, and How It May Bear on Shape Dynamics
Erik Curiel Ludwig-Maximilians-Universitiät München (LMU)
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Talk
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PSI 2016/2017 - Explorations in Quantum Gravity - Lecture 15
Maïté Dupuis Perimeter Institute for Theoretical Physics
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PSI 2016/2017 - Explorations in Quantum Gravity - Lecture 14
Maïté Dupuis Perimeter Institute for Theoretical Physics
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PSI 2016/2017 - Explorations in Quantum Gravity - Lecture 13
Maïté Dupuis Perimeter Institute for Theoretical Physics
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PSI 2016/2017 - Explorations in Quantum Gravity - Lecture 12
Maïté Dupuis Perimeter Institute for Theoretical Physics
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PSI 2016/2017 - Explorations in Quantum Gravity - Lecture 11
Maïté Dupuis Perimeter Institute for Theoretical Physics
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PSI 2016/2017 - Explorations in Quantum Gravity - Lecture 10
Maïté Dupuis Perimeter Institute for Theoretical Physics
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PSI 2016/2017 - Explorations in Quantum Gravity - Lecture 9
Maïté Dupuis Perimeter Institute for Theoretical Physics
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PSI 2016/2017 - Explorations in Quantum Gravity - Lecture 8
Maïté Dupuis Perimeter Institute for Theoretical Physics
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Talk
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PSI 2016/2017 - Relativity - Lecture 14
Neil Turok University of Edinburgh
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PSI 2016/2017 - Relativity - Lecture 13
Neil Turok University of Edinburgh
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PSI 2016/2017 - Relativity - Lecture 12
Neil Turok University of Edinburgh
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PSI 2016/2017 - Relativity - Lecture 11
Neil Turok University of Edinburgh
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PSI 2016/2017 - Relativity - Lecture 10
Neil Turok University of Edinburgh
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PSI 2016/2017 - Relativity - Lecture 9
Neil Turok University of Edinburgh
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PSI 2016/2017 - Relativity - Lecture 7
Neil Turok University of Edinburgh
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Talk
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Gravity Basics - 1
Veronika Hubeny University of California, Davis
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QI Basics - 1
Patrick Hayden Stanford University
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Entanglement - 1
Robert Spekkens Perimeter Institute for Theoretical Physics
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Bell’s Theorem
Adrian Kent University of Cambridge
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GR: Actions and Equations
David Kubiznak Charles University
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A new perspective on holographic entanglement
Matthew Headrick Brandeis University
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QI Basics - 2
John Watrous IBM (Canada)
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Talk
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Welcome and Opening Remarks
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Marina Cortes Institute for Astrophysics and Space Sciences
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Lee Smolin Perimeter Institute for Theoretical Physics
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Neil Turok University of Edinburgh
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The origin of arrows of time II
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Sean Carroll California Institute of Technology (Caltech) - Division of Physics Mathematics & Astronomy
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Marina Cortes Institute for Astrophysics and Space Sciences
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Tim Koslowski Technical University of Applied Sciences Würzburg-Schweinfurt
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The origin of arrows of time II cont.
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Sean Carroll California Institute of Technology (Caltech) - Division of Physics Mathematics & Astronomy
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Marina Cortes Institute for Astrophysics and Space Sciences
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Tim Koslowski Technical University of Applied Sciences Würzburg-Schweinfurt
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Testing time asymmetry in the early universe
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Brian Keating University of California, San Diego
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Andrew Liddle University of Lisbon
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Richard Muller University of California, Berkeley
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The fate of the big bang
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Abhay Ashtekar Pennsylvania State University
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Neil Turok University of Edinburgh
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Time as Organization – Downward Caustation, Structure and Complexity I
Barbara Drossel Technische Universität Darmstadt
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Time as Organization – Downward Caustation, Structure and Complexity II
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Stuart Kauffman Santa Fe Institute
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George Ellis University of Cape Town
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Talk
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Gravity Dual of Quantum Information Metric
Tadashi Takayanagi Yukawa Institute for Theoretical Physics
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A new perspective on holographic entanglement
Matthew Headrick Brandeis University
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Universal holographic description of CFT entanglement entropy
Thomas Faulkner University of Illinois Urbana-Champaign
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Geometric Constructs in AdS/CFT
Veronika Hubeny University of California, Davis
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Do black holes create polyamory
Jonathan Oppenheim University College London
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Tensor Network Renormalization and the MERA
Glen Evenbly Georgia Institute of Technology
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Entanglement renormalization for quantum fields
Jutho Haegeman Ghent University
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Holographic quantum error-correcting codes: Toy models for the bulk/boundary correspondence
Fernando Pastawski California Institute of Technology
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Talk
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Welcome to Perimeter Institute and the EHT 2014 Conference
Neil Turok University of Edinburgh
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Introduction to EHT
Shep Doeleman Harvard University
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Growth of supermassive black holes and their relationships to their host galaxies
Marta Volonteri Institut d'Astrophysique de Paris
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Polarized emission from Black Hole Accretion Disks and Jets
Jonathan McKinney University of Maryland, College Park
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Stellar Orbits at the Galactic Center
Andrea Ghez University of California, Los Angeles
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The Size and Morphology of Sgr A* at 7mm
Geoff Bower Academia Sinica
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Particle Acceleration and Non-thermal Emission in Radiatively Inefficient Accretion Flows
Eliot Quataert University of California, Berkeley
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Particle Acceleration in Magnetically-Dominated Turbulence
Rostom Mbarek University of Maryland, College Park
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Lecture - Strong Gravity, PHYS 777
William East Perimeter Institute for Theoretical Physics
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GRMHD simulations of accretion disks: QPOs, truncated disks and QPOs from truncated disks
Gibwa Musoke Canadian Institute for Theoretical Astrophysics
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PSI 2016/2017 - Explorations in Quantum Gravity (Dupuis)
PSI 2016/2017 - Explorations in Quantum Gravity (Dupuis) -
PSI 2016/2017 - Relativity (Turok)
PSI 2016/2017 - Relativity (Turok) -
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Quantum Information in Quantum Gravity II
Quantum Information in Quantum Gravity II -
Particle Acceleration in Magnetically-Dominated Turbulence
Rostom Mbarek University of Maryland, College Park
Building on recent advancements in understanding particle transport in magnetized media, we present a first-principles scaling law for the formation of non-thermal tails in particle spectra within mildly and strongly magnetized turbulent plasmas. This scaling is validated using results from kinetic Particle-In-Cell simulations, which show excellent agreement with our theoretical predictions. Finally, we discuss the astrophysical implications of these findings, particularly for the proton spectra in the coronae of supermassive black holes. -
Fast radio bursts as precursor radio emission from monster shocks
Amir LevinsonIt has been proposed recently that the breaking of MHD waves in the inner magnetosphere of strongly magnetized neutron stars can power different types of high-energy transients. We have studied the steepening and dissipation of a strongly magnetized fast magnetosonic wave propagating in a declining background magnetic field, by means of particle-in-cell simulations that encompass MHD scales. Our analysis confirms the formation of a monster shock as $B^2-E^2$ approaches zero, that dissipates about half of the fast magnetosonic wave energy, and reveals, for the first time, the generation of a high-frequency precursor wave at the monster shock, carrying a fraction of 0.001 of the total energy dissipated at the shock. The spectrum of the precursor wave exhibits several sharp harmonic peaks, with frequencies in the GHz band under conditions anticipated in magnetars. Such signals may appear as fast radio bursts. -
Modeling X-ray emission in radiation-rich magnetar magnetospheres
Jens Mahlmann Dartmouth College
Neutron star magnetospheres are a source of abundant X-ray activity. They have transients observed in different bands, like the fast radio burst (FRB) and associated hard X-ray flare from the Galactic magnetar SGR 1935+2154. We present global models for magnetar X-ray emission, including a landmark first-principle radiative particle-in-cell simulation of the twisted magnetar magnetosphere with the GPU-PIC code Entity. In one scenario, plasma particles accelerated by surface-motion-induced discharges interact resonantly with thermal background photons. Our GPU-accelerated particle-in-cell simulations track up-scattered high-energy photons that drive secondary pair production and ignite a magnetospheric circuit that persistently generates X-rays. We divulge the plasma properties of such a magnetospheric circuit, including densities and velocities, and give an outlook on alternative ignition scenarios for persistent magnetar X-ray emission. -
Lecture - Strong Gravity, PHYS 777
William East Perimeter Institute for Theoretical Physics
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GRMHD simulations of accretion disks: QPOs, truncated disks and QPOs from truncated disks
Gibwa Musoke Canadian Institute for Theoretical Astrophysics
Black hole X-ray binaries (BHXRBs) and Active Galactic Nuclei (AGN) transition through a series of accretion states in a well-defined order. The accretion states, each associated with different luminosities, spectral and variability characteristics, quasi periodic oscillations (QPOs) and outflow properties, are thought to be triggered by physical changes in the accretion disk around the central black hole.The mechanisms behind state transitions, the geometry of transitional disks and the physical mechanisms driving the emission characteristics we observe remain highly debated. General relativistic magneto-hydrodynamic simulations (GRMHD) are increasingly providing crucial insights into the accretion process, the launch of outflows and the physical processes driving state transitions in BHXRBs and AGN. Using GRMHD simulations conducted with the H-AMR code I: 1) Discuss how high and low-frequency QPOs can be produced by a highly tilted, geometrically thin accretion disk. 2) Present the first GRMHD simulation showing the self-consistent formation of a truncated accretion disk– a proposed disk model for the hard intermediate accretion state, in which the accretion flow is thick and hot close to the black hole, while the outer regions of the flow are thin and cool. 3) Describe how QPOs can be generated at the truncation radius (the radius at which the disk transitions from thick to thin) in a truncated accretion disk.