Vacuum polarization of the quantized massive fields in Friedman-Robertson-Walker spacetime

Matyjasek, Jerzy; Sadurski, Paweł; Telecka, Małgorzata

doi:10.1103/physrevd.89.084055

Cited by 12 publications

(18 citation statements)

References 33 publications

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“…The stress-energy tensor have been calculated in numerous, physically interesting geometries, such as exterior and interior regions of black holes [21,22], wormholes [23] and cosmology [24,25]. Interesting results have been obtained in the geometries with maximally symmetric subspaces, such as the Bertotti-Robinson solution [26][27][28].…”

Section: The Stress-energy Tensormentioning

confidence: 99%

“…To demonstrate that the components of the stress-energy tensor (20)(21)(22)(23)(24)(25)(26)(27) do satisfy this requirement let us introduce the vectors of the frame defined as follows. For radial motion the frame consists of the N -velocity vector e a (0) = u a and a unit length spacelike vector e a (1) = n a .…”

Section: The Intermediate Calculations Of T (N )A Bmentioning

confidence: 99%

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Stress-energy tensor of the quantized massive fields in Schwarzschild-Tangherlini spacetimes: The backreaction

Matyjasek

Sadurski²

2015

Phys. Rev. D

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We construct and study the approximate stress-energy tensor of the quantized massive scalar field in higher dimensional Schwarzschild-Tangherlini spacetimes. The stress-energy tensor is calculated within the framework of the Schwinger-DeWitt approach. It is shown that in N -dimensional spacetime the main approximation can be obtained from the effective action constructed form the coincidence limit of the Hadamard-DeWitt coefficient a k , where k − 1 is the integer part of N/2. The back reaction of the quantized field upon the black hole spacetime is analyzed and the quantum-corrected Komar mass and the Hawking temperature is calculated. It is shown that for the minimal and conformal coupling the increase of the Komar mass of the quantum corrected black hole leads to the decrease of its Hawking temperature. This is not generally true for more exotic values of the coupling parameter. The general formula describing the vacuum polarization, φ 2 , is constructed and briefly examined.

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Section: The Stress-energy Tensormentioning

confidence: 99%

Section: The Intermediate Calculations Of T (N )A Bmentioning

confidence: 99%

Stress-energy tensor of the quantized massive fields in Schwarzschild-Tangherlini spacetimes: The backreaction

Matyjasek

Sadurski²

2015

Phys. Rev. D

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“…Recently, the DeWitt-Schwinger point-splitting regularization [20][21][22][23][24], is used in [25,26] in the context of massive scalar, spinor and vector fields in spatially flat FLRW universe using asymptotic expansion of the Green function [17,27] to reproduce the leading order contribution to the stress tensor found in [28]. All these methods are equivalent [6].…”

Section: Introductionmentioning

confidence: 99%

Spin1/2field and regularization in a de Sitter and radiation dominated universe

Ghosh

2016

Phys. Rev. D

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We construct a simple algorithm to derive number density of spin 1/2 particles created in spatially flat FLRW spacetimes and resulting renormalized energy-momentum tensor within the framework of adiabatic regularization. Physical quantities thus found are in agreement with the known results. This formalism can be considered as an appropriate extension of the techniques originally introduced for scalar fields, applicable to fermions in curved space. We apply this formalism to compute the particle number density and the renormalized energy density and pressure analytically (wherever possible) and numerically, in two interesting cosmological scenarios: a de Sitter spacetime and a radiation dominated universe. Results prove the efficiency of the methodology presented here.

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“…In the context of the present paper, the most important are the studies of the quantized fields in cosmology (see e.g., Refs. [9][10][11][12][13][14][15][16][17][18][19][20][21][22] and the references cited therein) and the black hole interiors [23][24][25]. However, special emphasis -and it is natural -is put on the four dimensional calculations.…”

Section: Introductionmentioning

confidence: 99%

“…In this note, we shall calculate φ 2 of the quantized massive scalar field in the N -dimensional spatially flat Friedman-Robertson-Walker spacetime (FRW) using two distinctive techniques: explicit construction of the adiabatic modes on the one hand [11][12][13][14][15][16][20][21][22] and the calculations carried out within the framework of the Schwinger-DeWitt technique, heavily dependent on the heat kernel coefficients, on the other [21,22,29,[32][33][34][35][36][37]. We shall concentrate on the cosmological models satisfying 4 ≤ N ≤ 12 and briefly analyze the case of the lower-dimensional geometry.…”

Section: Introductionmentioning

confidence: 99%

Vacuum Polarization in Spatially-flat $N$-dimensional Friedman--Robertson--Walker Spacetimes

Matyjasek¹,

Sadurski²

2014

Acta Phys. Pol. B

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We investigate the vacuum polarization, φ 2 , of the quantized massive scalar field with a general curvature coupling parameter in the spatially-flat N -dimensional Friedman-Robertson-Walker spacetime with 4 ≤ N ≤ 12. The vacuum polarization is constructed using both adiabatic and Schwinger-DeWitt approaches and the full final results up to N = 7 are explicitly demonstrated. The behavior of φ 2 for 4 ≤ N ≤ 12 is examined in the exponentially expanding universe, in the power-law and inflationary powerlaw models. In the case of exponential expansion, φ 2 is constant and for a given mass it depends solely on the Hubble constant and the curvature coupling parameter. In the power-law models its behavior is more complicated and, generally, decays in time as t −n , where n/2 is the integer part of N/2. The 2 + 1-dimensional case is also briefly analyzed. The relevance of the present results to the stress-energy tensor is examined.

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Vacuum polarization of the quantized massive fields in Friedman-Robertson-Walker spacetime

Cited by 12 publications

References 33 publications

Stress-energy tensor of the quantized massive fields in Schwarzschild-Tangherlini spacetimes: The backreaction

Stress-energy tensor of the quantized massive fields in Schwarzschild-Tangherlini spacetimes: The backreaction

Spin1/2field and regularization in a de Sitter and radiation dominated universe

Vacuum Polarization in Spatially-flat $N$-dimensional Friedman--Robertson--Walker Spacetimes

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