Quantum quenches in free field theory: universal scaling at any rate

Das, Sumit R.; Galante, Damián A.; Myers, Robert C.

doi:10.1007/jhep05(2016)164

Cited by 42 publications

(80 citation statements)

References 43 publications

(276 reference statements)

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“…(3.43) shows no dependence on ct at all, and so this points to another mismatch between the holographic and QFT results. One possible way to improve the comparison of the holographic and QFT quenches would be to consider CFT-to-CFT quenches for a free scalar (in which the initial and final masses both vanish) using the protocol described in section 3.2 of [88]. Another simple extension of this work would be to study the complexity for a mass quench of a free fermion, using the techniques of [46].…”

Section: Jhep06(2018)046mentioning

confidence: 99%

“…In these geometries describing a one-sided black hole, we evaluate the holographic complexity, using the Complexity=Action proposal in section 3.1, and the Complexity=Volume proposal in section 3.2. From the perspective of the boundary CFT, this geometry describes a quantum quench, e.g., see [62][63][64][65][86][87][88]. The CFT begins in the vacuum state and then, say, at t = 0, we act with a (homogeneous) operator which injects energy into the system creating an excited state.…”

Section: Jhep06(2018)046mentioning

confidence: 99%

“…Some initial studies of this question appear in [98,99], which examine the evolution of the complexity through a mass quench in a free scalar field theory (analogous to those studied in [86][87][88]). A remarkable feature of these quenches is that the scalar field remains in a Gaussian state throughout the entire process, and so methods developed in [44][45][46] can still be applied to evaluate the complexity.…”

Section: Future Directionsmentioning

confidence: 99%

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Holographic complexity in Vaidya spacetimes. Part I

Chapman

Marrochio

Myers

2018

J. High Energ. Phys.

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150

222

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We examine holographic complexity in time-dependent Vaidya spacetimes with both the complexity=volume (CV) and complexity=action (CA) proposals. We focus on the evolution of the holographic complexity for a thin shell of null fluid, which collapses into empty AdS space and forms a (one-sided) black hole. In order to apply the CA approach, we introduce an action principle for the null fluid which sources the Vaidya geometries, and we carefully examine the contribution of the null shell to the action. Further, we find that adding a particular counterterm on the null boundaries of the Wheeler-DeWitt patch is essential if the gravitational action is to properly describe the complexity of the boundary state. For both the CV proposal and the CA proposal (with the extra boundary counterterm), the late time limit of the growth rate of the holographic complexity for the one-sided black hole is precisely the same as that found for an eternal black hole.

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Section: Jhep06(2018)046mentioning

confidence: 99%

Section: Jhep06(2018)046mentioning

confidence: 99%

Section: Future Directionsmentioning

confidence: 99%

See 1 more Smart Citation

Holographic complexity in Vaidya spacetimes. Part I

Chapman

Marrochio

Myers

2018

J. High Energ. Phys.

Self Cite

150

222

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“…See Refs. [59][60][61][62][63][64][65][66] for more details in this direction. In this context we are interested in this specific type of mass parametrization as the corresponding equivalent version of Schrödinger quantum mechanical problem can easily solvable.…”

Section: Creation Of New Massive Particlementioning

confidence: 99%

Bell violation in the sky

2017

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In this work, we have studied the possibility of setting up Bell's inequality violating experiment in the context of cosmology, based on the basic principles of quantum mechanics. First we start with the physical motivation of implementing the Bell inequality violation in the context of cosmology. Then to set up the cosmological Bell violating test experiment we introduce a model independent theoretical framework using which we have studied the creation of new massive particles by implementing the WKB approximation method for the scalar fluctuations in the presence of additional time-dependent mass contribution in the cosmological perturbation theory. Here for completeness we compute the total number density and the energy density of the newly created particles in terms of the Bogoliubov coefficients using the WKB approximation method. Next using the background scalar fluctuation in the presence of a new time-dependent mass contribution, we explicitly compute the expression for the one point and two point correlation functions. Furthermore, using the results for a one point function we introduce a new theoretical cosmological parameter which can be expressed in terms of the other known inflationary observables and can also be treated as a future theoretical probe to break the degeneracy amongst various models of inflation. Additionally, we also fix the scale of inflation in a model-independent way without any prior knowledge of primordial gravitational waves. Also using the input from a newly introduced cosmological parameter, we finally give a theoretical estimate for the tensor-to-scalar ratio in a modelindependent way. Next, we also comment on the technicalities of measurements from isospin breaking interactions and the future prospects of newly introduced massive particles in a cosmological Bell violating test experiment. Further, we a

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“…Schematic descriptions of the mass potential m 2 (t) in the ECP and the CCP. We will explain the ECP and CCP in more details in section 2. functions, entanglement measures, and complexity in the ECP and CCP were studied in [6][7][8][9][10][11][12][13][14][15][16].…”

Section: Introductionmentioning

confidence: 99%

Entanglement after quantum quenches in Lifshitz scalar theories

Kim¹,

Nishida²,

Seo³

et al. 2019

J. Stat. Mech.

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We study the time evolution of the entanglement entropy after quantum quenches in Lifshitz free scalar theories, with the dynamical exponent z > 1, by using the correlator method. For quantum quenches we consider two types of time-dependent mass functions: end-critical-protocol (ECP) and cis-critical-protocol (CCP). In both cases, at early times the entanglement entropy is independent of the subsystem size. After a critical time (t c ), the entanglement entropy starts depending on the subsystem size significantly. This critical time t c for z = 1 in the fast ECP and CCP has been explained well by the fast quasi-particle of the quasi-particle picture. However, we find that for z > 1 this explanation does not work and t c is delayed. We explain why t c is delayed for z > 1 based on the quasiparticle picture: in essence, it is due to the competition between the fast and slow quasiparticles. At late times, in the ECP, the entanglement entropy slowly increases while, in the CCP, it is oscillating with a well defined period by the final mass scale, independently of z. We give an interpretation of this phenomena by the correlator method. As z increases, the entanglement entropy increases, which can be understood by long-range interactions due to z. arXiv:1906.05476v2 [hep-th]

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Quantum quenches in free field theory: universal scaling at any rate

Cited by 42 publications

References 43 publications

Holographic complexity in Vaidya spacetimes. Part I

Holographic complexity in Vaidya spacetimes. Part I

Bell violation in the sky

Entanglement after quantum quenches in Lifshitz scalar theories

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