Induced vacuum current and magnetic field in the background of a cosmic string

Sitenko, Yu. A.; Власій, Н. Д.

doi:10.1088/0264-9381/26/19/195009

Cited by 34 publications

(34 citation statements)

References 65 publications

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“…2 Additionally to the contribution for the energy-momentum tensor associated with charged quantum fields, the presence of a magnetic flux along the cosmic string induces vacuum current densities, as well. This phenomenon has been investigated for massless scalar field in [28] and recently for massive one in [29]. There the authors have shown that a vacuum induced azimuthal current densities, j ϕ , take place if the ratio of the magnetic flux by the quantum one has a non-vanishing fractional part.…”

Section: Introductionmentioning

confidence: 98%

Induced fermionic current densities by magnetic flux in higher dimensional cosmic string spacetime

Mello¹

2010

Class. Quantum Grav.

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In this paper we analyse the vacuum fluctuations of quantum fermionic current densities, j A (x) , induced by a magnetic flux running along the core of the conical space produced by the presence of cosmic string, in a (1 + d)−dimensional bulk, for 2 ≤ d ≤ 5. In order to develop this investigation we construct an expression for the fermionic propagator, which can be applied for those different dimensions of the spacetime. Two specific analysis for the induced current densities are presented: (i) for massless fields in three and four dimensions, and (ii) for massive fields in all dimensions considered. In the latter specific values for the parameters which codify the presence of the cosmic string and the fractional part of the ratio of the magnetic flux by the quantum one are considered. Although being a very special situation and somewhat unnatural, the corresponding analysis of induced fermionic current densities under this circumstance may shed light on the qualitative behavior of these quantities in a more general situation.

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Section: Introductionmentioning

confidence: 98%

Induced fermionic current densities by magnetic flux in higher dimensional cosmic string spacetime

Mello¹

2010

Class. Quantum Grav.

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“…The presence of a magnetic flux induces also vacuum current densities. This phenomenon was analyzed for massless [33] and massive [34] scalar fields. It has been shown that an azimuthal vacuum current appears if the ratio of the magnetic flux by the quantum one has a nonzero fractional part.…”

Section: Introductionmentioning

confidence: 99%

Induced fermionic currents in de Sitter spacetime in the presence of a compactified cosmic string

Mohammadi

Mello

Saharian

2015

Class. Quantum Grav.

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We investigate the vacuum fermionic currents in the geometry of a compactified cosmic string on background of de Sitter spacetime. The currents are induced by magnetic fluxes running along the cosmic string and enclosed by the compact dimension. We show that the vacuum charge and the radial component of the current density vanish. By using the Abel-Plana summation formula, the azimuthal and axial currents are explicitly decomposed into two parts: the first one corresponds to the geometry of a straight cosmic string and the second one is induced by the compactification of the string along its axis. For the axial current the first part vanishes and the corresponding topological part is an even periodic function of the magnetic flux along the string axis and an odd periodic function of the flux enclosed by the compact dimension with the periods equal to the flux quantum. The azimuthal current density is an odd periodic function of the flux along the string axis and an even periodic function of the flux enclosed by the compact dimension with the same period. Depending on the magnetic fluxes, the planar angle deficit can either enhance or reduce the azimuthal and axial currents. The influence of the background gravitational field on the vacuum currents is crucial at distances from the string larger than the de Sitter curvature radius. In particular, for the geometry of a straight cosmic string and for a massive fermionic field, we show that the decay of the azimuthal current density is damping oscillatory with the amplitude inversely proportional to the fourth power of the distance from the string. This behavior is in clear contrast with the case of the string in Minkowski bulk where the current density is exponentially suppressed at large distances.

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“…To construct the complete set of the wave-functions we will consider (13) in the regions r < a and r > a, separately. For the inner region, we have three different configurations of magnetic field given by (5)- (9), as we showed previously.…”

Section: The Geometry and The Fermionic Wave-functionsmentioning

confidence: 99%

“…Consequently, there will be three different solutions for (13). Let us define each radial function represented by R (i) l , where we introduced i = 1, 2, 3, the index associated with the model and l = 1, 2 the index associated to the spinor components.…”

Section: The Geometry and The Fermionic Wave-functionsmentioning

confidence: 99%

“…Considering the presence of the magnetic flux, additional polarization effects take place, these ones associated with charged quantum fields, as we can see in [6][7][8][9][10][11]. Specifically speaking the magnetic flux induces a non-zero azimuthal current densities, j φ (see references [12,13]). Although the results found for these currents are calculated considering a fixed configuration of magnetic field, these currents act as sources of the semiclassical Maxwell's equations and play important roles in modeling a self-consistent dynamics involving the electromagnetic fields.…”

Section: Introductionmentioning

confidence: 97%

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Azimuthal Fermionic Current in the Cosmic String Spacetime Induced by a Magnetic Tube

2018

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Abstract:In this paper, we calculate the vacuum expectation value of the azimuthal fermionic current, associated with a massive fermionic quantum field in the spacetime of an idealized cosmic string, considering the presence of a magnetic tube of radius a, coaxial to the string. In this analysis three distinct configurations of magnetic field are considered: (i) a magnetic field concentrated on a surface of the tube; (ii) a magnetic field presenting a 1/r radial dependence; and (iii) an homogeneous magnetic field. In order to develop this analysis , we construct the complete set of normalized solution of the Dirac equation in the region outside the tube. By using the mode-sum formula, we show that the azimuthal induced current is formed by two contributions: the first being the current induced by a line of magnetic flux running along the string, and the second, named core-induced current, is induced by the non-vanishing extension of the magnetic tube. The first contribution depends only on the fractional part of the ration of the magnetic flux inside the tube by the quantum one; as to the second contribution, it depends on the total magnetic flux. We specifically analyze the core-induced current in several limits of the parameters and distance to the tube.

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Induced vacuum current and magnetic field in the background of a cosmic string

Cited by 34 publications

References 65 publications

Induced fermionic current densities by magnetic flux in higher dimensional cosmic string spacetime

Induced fermionic current densities by magnetic flux in higher dimensional cosmic string spacetime

Induced fermionic currents in de Sitter spacetime in the presence of a compactified cosmic string

Azimuthal Fermionic Current in the Cosmic String Spacetime Induced by a Magnetic Tube

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