Fractional brane state in the early Universe

Chowdhury, Borun D.; Mathur, Samir D.

doi:10.1088/0264-9381/24/10/014

Cited by 44 publications

(130 citation statements)

References 64 publications

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“…If so, the wavefunction spread over this vast phase space can change classical dynamics by order unity, and in particular may resolve the initial singularity in the same way that we have avoided the black hole central singularity. Some initial considerations in this direction are discussed in [48].…”

Section: Discussionmentioning

confidence: 99%

Black holes and beyond

Mathur

2012

Annals of Physics

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The black hole information paradox forces us into a strange situation: we must find a way to break the semiclassical approximation in a domain where no quantum gravity effects would normally be expected. Traditional quantizations of gravity do not exhibit any such breakdown, and this forces us into a difficult corner: either we must give up quantum mechanics or we must accept the existence of troublesome 'remnants'. In string theory, however, the fundamental quanta are extended objects, and it turns out that the bound states of such objects acquire a size that grows with the number of quanta in the bound state. The interior of the black hole gets completely altered to a 'fuzzball' structure, and information is able to escape in radiation from the hole. The semiclassical approximation can break at macroscopic scales due to the large entropy of the hole: the measure in the path integral competes with the classical action, instead of giving a subleading correction. Putting this picture of black hole microstates together with ideas about entangled states leads to a natural set of conjectures on many long-standing questions in gravity: the significance of Rindler and de Sitter entropies, the notion of black hole complementarity, and the fate of an observer falling into a black hole.

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Section: Discussionmentioning

confidence: 99%

Black holes and beyond

Mathur

2012

Annals of Physics

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“…Through this picture we will find that we have one conserved quantity and this give us a first constraint in the Hamiltonian formulation. We start by looking for the Lagrangian density for the matter content, and this is given by a perfect fluid as a first approximation in this formalism, whose stress-energy tensor is [22,23] …”

Section: Classical Lagrangian and Hamiltonianmentioning

confidence: 99%

Cosmologies with Scalar Fields from Higher Dimensions Applied to Bianchi Type VIh=-1 Model: Classical and Quantum Solutions

Socorro

Sesma

Pimentel

2018

Advances in High Energy Physics

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We construct an effective four-dimensional model by compactifying a ten-dimensional theory of gravity coupled with a real scalar dilaton field on a time-dependent torus. The corresponding action in four dimensions is similar to the action of K-essence theories. This approach is applied to anisotropic cosmological Bianchi type (ℎ=−1) model for which we study the classical coupling of the anisotropic scale factors with the two real scalar moduli produced by the compactification process. The classical Einstein field equations give us a hidden symmetry, corresponding to the equality between two radii B=C, which permits us to solve exactly the equations of motion. One relation between the scale factors (A,C) via the solutions is found. With this hidden symmetry, then we solve the FRW model, finding that the scale factor goes to B radii. Also the corresponding Wheeler-DeWitt (WDW) equation in the context of Standard Quantum Cosmology is solved, building a wavepacket when the scalar fields have a hyperbolic behavior, obtaining some qualitative results when we analyze the projection plane to the wall formed by the probability density. Bohm's formalism for this cosmological model is revisited too.

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“…We propose that the qualitative effects of the nonlocal dynamics can be tucked into initial conditions for the standard equations of evolution for small fluctuations. This is known in the cosmology literature as the minimal approach [25][26][27] (for other recent and interesting realizations of string cosmology, see for example [28][29][30][31][32][33][34][35][36][37][38]). …”

Section: Application To Cosmologymentioning

confidence: 99%

New mechanism for nonlocality from string theory: UV-IR quantum entanglement and its imprints on the CMB

Minton

Sahakian

2008

Phys. Rev. D

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New mechanism for nonlocality from string theory: UV-IR quantum entanglement and its imprints on the CMB." Phys. Rev. D 77, 026008 (2008).New mechanism for nonlocality from string theory: UV-IR quantum entanglement and its imprints on the CMB Puff field theories (PFT) arise as the decoupling limits of D3 branes in a Melvin universe and exhibit spatially nonlocal dynamics. Unlike other realizations of nonlocality in string theory, PFTs have full SO 3 rotational symmetry. In this work, we analyze the strongly coupled regime of a PFT through gravitational holography. We find a novel mechanism at the heart of the phenomenon of nonlocality: a quantum entanglement of UV and IR dynamics. In the holographic bulk, this translates to an apparent horizon splitting the space into two regions-with the UV completion of the PFT sitting at the horizon. We unravel this intricate UV-IR setting and devise a prescription for computing correlators that extends the original dictionary of holographic renormalization group. We then implement a cosmological scenario where PFT correlators set the initial conditions for primordial fluctuations. We compute the associated power spectrum of the cosmic microwave background and find that the scenario allows for a distinct stringy signature.

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Fractional brane state in the early Universe

Cited by 44 publications

References 64 publications

Black holes and beyond

Black holes and beyond

Cosmologies with Scalar Fields from Higher Dimensions Applied to Bianchi Type VIh=-1 Model: Classical and Quantum Solutions

New mechanism for nonlocality from string theory: UV-IR quantum entanglement and its imprints on the CMB

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