Neutrino currents in wakes of cosmic strings

Sau, Sovan; Sanyal, Sankar P.

doi:10.1140/epjc/s10052-020-7734-z

Cited by 8 publications

(12 citation statements)

References 42 publications

(29 reference statements)

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“…The presence of magnetic reconnection can be understood from the fact that we have pressure changes in the cosmic string wakes coupled with the fact that the generated magnetic field is perpendicular to the flow direction and is also oscillatory in nature. As mentioned before the form of the magnetic field is mo- tivated by the magnetic field generated by neutrino gradients around Abelian Higgs cosmic strings [5]. The neutrino gradients cause electron gradients in the plasma due to electron-neutrino interactions.…”

Section: Reconnection In the Wakes Of The Cosmic Stringmentioning

confidence: 94%

“…It is given by B = B 0 exp(−Ay)cos(ωy)ŷ The form is motivated by the nature of the magnetic field generated in ref. [5] and the symmetry of the problem. The magnetic field generated is perpendicular to the direction of motion of the cosmic string.…”

Section: Boundary Conditions and Magnetohydrodynamic Equationsmentioning

confidence: 99%

“…This method will generate a magnetic field whenever the temperature gradient and the density gradient in an inhomogeneous plasma are not aligned to each other. Though this can happen under various circumstances in the early universe, we are interested in the magnetic fields that are generated in the wakes of cosmic strings [5].…”

Section: Introductionmentioning

confidence: 99%

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Evolution of magnetic fields in cosmic string wakes

Nayak¹,

Sau²,

Sanyal³

2022

Preprint

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We study the evolution of magnetic fields in cosmic string wakes in a plasma with a low resistivity. The initial magnetic field in the wake is modelled on the magnetic fields that are generated by the motion of particles around cosmic strings. The plasma is characterized by a high beta value. We find multiple shock like structures developing in the wake of the string. We study the detailed structure of the shocks formed and the evolution of the magnetic field in the shock using a 2-D magnetohydrodynamic simulation. As expected, the developement of the magnetic field does not depend on the β value. Our results show that instead of a singe uniform shock forming behind the cosmic string we have multiple shocks forming at short time intervals behind the string. The presence of multiple shocks will definitely affect the obsevational signatures of cosmic string wakes as these signatures depend upon the temperature fluctuations generated by the shock. We also find that as the shock moves away, the residual magnetic field left behind reconnects and dissipates rapidly. The magnetic field around the string is thus very localized. We find that magnetic field reconnections take place in cosmic string wakes. This leads to the decrease of the magnetic field in the post shock region.

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Section: Reconnection In the Wakes Of The Cosmic Stringmentioning

confidence: 94%

Section: Boundary Conditions and Magnetohydrodynamic Equationsmentioning

confidence: 99%

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Evolution of magnetic fields in cosmic string wakes

Nayak¹,

Sau²,

Sanyal³

2022

Preprint

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“…The detailed discussion on magnetic field generation by neutrino currents in cosmic string wakes may be obtained from ref. [14].…”

Section: Sovan Saumentioning

confidence: 99%

Generation of magnetic fields in cosmic string wakes

Sau¹,

Sanyal²

2021

Proceedings of 40th International Conference on High Energy Physics — PoS(ICHEP2020)

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We describe a novel method of generating magnetic fields in cosmic string wakes from neutrino currents. We show that neutrino currents act as a cross-perturbation across the cosmic string wake. This cross perturbation along with the high Reynolds number generates a magnetic field in the wake of the cosmic string. The neutrino current is generated by the neutrinos rotating around the Abelian Higgs strings. As the string moves through the cosmic plasma, the velocity kick generated by the motion of the string will enhance the neutrino current in the wake region. The neutrino current density depends on its distance from the string and is oscillatory in nature. This leads to neutrino density gradients in the plasma. We have shown that these neutrino gradients give rise to electron gradients in the plasma, which in turn generate magnetic fields of the order of 10 13 Gauss.

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“…In this case, the cosmic string need not be a superconducting cosmic string. Magnetic fields can be generated in the wake of Abelian Higgs string during the radiation epoch by the Biermann battery mechanism [9]. The Biermann mechanism generates the field when there are density inhomogeneities in the wake due to the motion of neutrinos around the cosmic string.…”

Section: Introductionmentioning

confidence: 99%

Magnetic reconnection in the wakes of cosmic strings

Kumar¹,

Sanyal²

2022

Preprint

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The motion of cosmic strings in the universe leads to the generation of wakes behind them. We study magnetized wakes of cosmic strings moving in the post recombination plasma. We show that magnetic reconnection can occur in the post shock region. Since the width of the cosmic string wake is very small, the reconnection occurs over a very short lengthscale. The reconnection leads to a large amount of kinetic energy being released in the post shock region of the cosmic string wake. This enhances the kinetic energy released during the reconnection. We make a rudimentary estimate of the kinetic energy released by the magnetic reconnection in cosmic strings wakes and show that it can account for low energy Gamma Ray Bursts (GRB) in the post recombination era.

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Neutrino currents in wakes of cosmic strings

Cited by 8 publications

References 42 publications

Evolution of magnetic fields in cosmic string wakes

Evolution of magnetic fields in cosmic string wakes

Generation of magnetic fields in cosmic string wakes

Magnetic reconnection in the wakes of cosmic strings

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