On Computation of Some Asymptotic Characteristics of Vacuum Polarization in Schwarzschild Space-Time

2000 ◽  
pp. 719-726
Author(s):  
Juri M. Rappoport
Keyword(s):  
Vacuum Polarization ◽  
Space Time

THE MICROSCOPIC-MACROSCOPIC SCALE TRANSFORMATION THROUGH A CHAOS SCENARIO IN THE FRACTAL SPACE-TIME THEORY

2011 ◽  
Vol 21 (02) ◽  
pp. 603-618 ◽  
Author(s):  
G. V. MUNCELEANU ◽  
V.-P. PAUN ◽  
I. CASIAN-BOTEZ ◽  
M. AGOP
Keyword(s):  
Vacuum Polarization ◽  
Plasma Plume ◽  
Space Time ◽  
Time Dependent ◽  
Scale Transformation ◽  
Particle Movement ◽  
Specific Mechanism ◽  
Macroscopic Scale ◽  
Fractal Space ◽  
Time Theory

Considering that the particle movement takes place on fractal curves, the mathematical and physical aspects in fractal space-time theory are analyzed. In such context, the harmonic oscillator problem implies that the microscopic-macroscopic scale transition could be associated with an evolution scenario towards chaos. The splitting of the plasma plume, generated by laser ablation, into two patterns, has been successfully reproduced through a numerical simulation using the fractal hydrodynamic model. For the free time-dependent particle in a fractal space-time, the uniform movement is naturally obtained by a specific mechanism of vacuum polarization.

scholarly journals Vacuum polarization in Schwarzschild space-time by anomaly induced effective actions

1999 ◽  
Vol 559 (1-2) ◽  
pp. 301-319 ◽  
Author(s):  
R. Balbinot ◽  
A. Fabbri ◽  
I. Shapiro
Keyword(s):  
Vacuum Polarization ◽  
Space Time

scholarly journals VACUUM POLARIZATION IN THE SPACE–TIME OF A SCALAR–TENSOR COSMIC STRING

2001 ◽  
Vol 16 (24) ◽  
pp. 1565-1571 ◽  
Author(s):  
V. B. BEZERRA ◽  
R. M. TEIXEIRA FILHO ◽  
G. GREBOT ◽  
M. E. X. GUIMARÃES
Keyword(s):  
Cosmic String ◽  
Polarization Effect ◽  
Vacuum Polarization ◽  
Energy Momentum Tensor ◽  
Vacuum Expectation ◽  
Momentum Tensor ◽  
Space Time ◽  
Scalar Tensor Theory ◽  
Expectation Values ◽  
Tensor Theory

We study the vacuum polarization effect in the space–time generated by a magnetic flux cosmic string in the framework of a scalar–tensor theory of gravity. The vacuum expectation values of the energy–momentum tensor of a conformally coupled scalar field are calculated and the dilaton's contribution to the vacuum polarization effect is shown.

scholarly journals VACUUM POLARIZATION BY A MAGNETIC FLUX TUBE AT FINITE TEMPERATURE IN THE COSMIC STRING SPACE–TIME

2009 ◽  
Vol 18 (01) ◽  
pp. 53-70 ◽  
Author(s):  
J. SPINELLY ◽  
E. R. BEZERRA DE MELLO
Keyword(s):  
Magnetic Flux ◽  
Flux Tube ◽  
Cosmic String ◽  
Vacuum Polarization ◽  
Temperature Limit ◽  
Space Time ◽  
Magnetic Flux Tube ◽  
Massless Scalar ◽  
Homogeneous Field ◽  
Massless Scalar Field

In this paper, we analyze the effect produced by the temperature in the vacuum polarization associated with a charged massless scalar field in the presence of a magnetic flux tube in the cosmic string space–time. Three different configurations of magnetic fields are taken into account: (i) a homogeneous field inside the tube, (ii) a field proportional to 1/r, and (iii) a cylindrical shell with δ-function. In these three cases, the axis of the infinitely long tube of radius R coincides with the cosmic string. Because of the complexity of this analysis in the region inside the tube, we consider the thermal effect in the region outside. In order to develop this analysis, we construct the thermal Green function associated with this system for the three above-mentioned situations considering points in the region outside the tube. We explicitly calculate, in the high-temperature limit, the thermal average of the field square and the energy–momentum tensor.

scholarly journals CANCELLATION OF ULTRAVIOLET DIVERGENCES FOR LOCALLY FLAT METRICS

1998 ◽  
Vol 13 (38) ◽  
pp. 3081-3090
Author(s):  
M. HORTAÇSU ◽  
N. ÖZDEMIR
Keyword(s):  
General Class ◽  
Vacuum Polarization ◽  
Cosmic Strings ◽  
Scalar Particle ◽  
Space Time ◽  
Spinor Particle ◽  
Perturbative Calculation ◽  
Massless Field ◽  
The One ◽  
Work Done

We extend the work done for cosmic strings on the perturbative calculation of vacuum polarization of a massless field in the space–time of multiple cosmic strings and show that for a more general class of locally flat metrics, the one-loop calculation does not introduce any new divergences to the vev of the energy of a scalar particle or a spinor particle.

AMBIGUITIES AND SYMMETRY RELATIONS IN FIVE-DIMENSIONAL PERTURBATIVE CALCULATIONS: THE EXPLICIT EVALUATION OF THE QED5 VACUUM POLARIZATION TENSOR

2013 ◽  
Vol 28 (27) ◽  
pp. 1350135
Author(s):  
M. V. S. FONSECA ◽  
T. J. GIRARDI ◽  
G. DALLABONA ◽  
O. A. BATTISTEL
Keyword(s):  
Quantum Electrodynamics ◽  
Vacuum Polarization ◽  
Space Time ◽  
General Character ◽  
Polarization Tensor ◽  
Time Dimension ◽  
Perturbative Calculations ◽  
Explicit Evaluation ◽  
The One ◽  
Vacuum Polarization Tensor

An explicit evaluation of the D = 4+1 quantum electrodynamics (QED) vacuum polarization tensor is presented. The calculations are made preserving all the intrinsic arbitrariness involved in such type of problem. The internal momenta are assumed arbitrary in order to preserve the possibility of dependence on such kind of choice, due to the superficial degree of divergence involved. An arbitrary scale is introduced in the separation of terms having different degrees of divergences in order to preserve the possibility of scale ambiguities. In the performed steps the effects of regularizations are avoided by using an adequate strategy to handle the problem of divergences in Quantum Field Theory perturbative calculations. Given this attitude it is possible to get clean and sound conclusions about the consistency requirements involved in perturbative calculations D = 4+1 space–time dimension. At the final a symmetry preserving and ambiguities free result is obtained allowing the renormalization of the photon propagator at the one-loop level. The simplicity added to the general character of the adopted procedure allows us to believe that the referred strategy can be used without restrictions of applicability in perturbative calculations made in theories formulated in a space–time having extra dimensions relative to the physical one (D = 3+1) producing consistent results, in odd and even dimensions, in spite of the nonrenormalizable character.

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