scholarly journals Spinor Green function in higher-dimensional cosmic string space-time in the presence of magnetic flux

2008 ◽  
Vol 2008 (09) ◽  
pp. 005-005 ◽  
Author(s):  
J Spinelly ◽  
E.R. Bezerra de Mello
Keyword(s):  
Green Function ◽  
Magnetic Flux ◽  
Cosmic String ◽  
Space Time ◽  
Higher Dimensional

scholarly journals Induced vacuum bosonic current by magnetic flux in a higher dimensional compactified cosmic string spacetime

2015 ◽  
Vol 24 (07) ◽  
pp. 1550055 ◽  
Author(s):  
E. A. F. Bragança ◽  
H. F. Santana Mota ◽  
E. R. Bezerra de Mello
Keyword(s):  
Magnetic Flux ◽  
Current Density ◽  
Cosmic String ◽  
Axial Current ◽  
Asymptotic Expressions ◽  
Dimensional Spacetime ◽  
Arbitrary Phase ◽  
Higher Dimensional ◽  
Quantum Flux ◽  
Azimuthal Current

In this paper, we analyze the bosonic current densities induced by a magnetic flux running along an idealized cosmic string in a high-dimensional spacetime, admitting that the coordinate along the string's axis is compactified. Additionally we admit the presence of a magnetic flux enclosed by the compactification axis. In order to develop this analysis we calculate the complete set of normalized bosonic wave functions obeying a quasiperiodicity condition, with arbitrary phase β, along the compactified dimension. In this context, only azimuthal and axial currents densities take place. As to the azimuthal current, two contributions appear. The first contribution corresponds to the standard azimuthal current in a cosmic string spacetime without compactification, while the second contribution is a new one, induced by the compactification itself. The latter is an even function of the magnetic flux enclosed by the string axis and is an odd function of the magnetic flux along its core with period equal to quantum flux, Φ0 = 2π/e. On the other hand, the nonzero axial current density is an even function of the magnetic flux along the core of the string and an odd function of the magnetic flux enclosed by it. We also find that the axial current density vanishes for untwisted and twisted bosonic fields in the absence of the magnetic flux enclosed by the string axis. Some asymptotic expressions for the current density are provided for specific limiting cases of the physical parameter of the model.

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.

The spin-zero Duffin-Kemmer-Petiau equation in a cosmic-string space-time with the Cornell interaction

2016 ◽  
Vol 31 (36) ◽  
pp. 1650191 ◽  
Author(s):  
M. de Montigny ◽  
M. Hosseinpour ◽  
H. Hassanabadi
Keyword(s):  
Gravitational Field ◽  
Coordinate System ◽  
Cosmic String ◽  
Topological Defects ◽  
Space Time ◽  
Dkp Equation

In this paper, we study the covariant Duffin-Kemmer-Petiau (DKP) equation in the cosmic-string space-time and consider the interaction of a DKP field with the gravitational field produced by topological defects in order to examine the influence of topology on this system. We solve the spin-zero DKP oscillator in the presence of the Cornell interaction with a rotating coordinate system in an exact analytical manner for nodeless and one-node states by proposing a proper ansatz solution.

MANIFOLD-SPLITTING REGULARIZATION, SELF-LINKING, TWISTING, WRITHING NUMBERS OF SPACE-TIME RIBBONS and POLYAKOV’S PROOF OF FERMI-BOSE TRANSMUTATIONS

1988 ◽  
Vol 03 (08) ◽  
pp. 1959-1979 ◽  
Author(s):  
CHIA-HSIUNG TZE
Keyword(s):  
Integral Formula ◽  
Space Time ◽  
Gauge Fields ◽  
Alternative Formulation ◽  
Complex Numbers ◽  
Closed Space ◽  
Feynman Path ◽  
Higher Dimensional ◽  
Linking Coefficient ◽  
In Memoriam

We present an alternative formulation of Polyakov’s regularization of Gauss’ integral formula for a single closed Feynman path. A key element in his proof of the D=3 fermi-bose transmutations induced by topological gauge fields, this regularization is linked here with the existence and properties of a nontrivial topological invariant for a closed space ribbon. This self-linking coefficient, an integer, is the sum of two differential characteristics of the ribbon, its twisting and writhing numbers. These invariants form the basis for a physical interpretation of our regularization. Their connection to Polyakov’s spinorization is discussed. We further generalize our construction to the self-linking, twisting and writhing of higher dimensional d=n (odd) submanifolds in D=(2n+1) space-time. Our comprehensive analysis intends to supplement Polyakov’s work as it identifies a natural path to its higher dimensional mathematical and physical generalizations. Combining the theorems of White on self-linking of manifolds and of Adams on nontrivial Hopf fibre bundles and the four composition-division algebras, we argue that besides Polyakov’s case where (d, D)=(1, 3) tied to complex numbers, the potentially interesting extensions are two chiral models with (d, D)=(3, 7) and (7, 15) uniquely linked to quaternions and octonions. In Memoriam Richard P. Feynman

Relativistic star solutions in higher-dimensional pseudospheroidal space-time

Pramana ◽  
2010 ◽  
Vol 74 (4) ◽  
pp. 513-523 ◽  
Author(s):  
P. K. Chattopadhyay ◽  
B. C. Paul
Keyword(s):  
Space Time ◽  
Relativistic Star ◽  
Higher Dimensional
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