Magnetic field amplification and decay in cosmic string wakes

TL;DR

This paper investigates how magnetic fields are amplified or decay in the wakes of moving cosmic strings, revealing dependence on perturbation lengthscale and implications for magnetic reconnection in cosmic plasmas.

Contribution

It provides a detailed analytical and numerical analysis of magnetic field behavior in cosmic string wakes, highlighting the role of perturbation lengthscale and plasma properties.

Findings

Magnetic field amplification occurs in cosmic string wakes due to overdensity effects.

Decay of magnetic fields can happen when perturbation lengthscale exceeds the gyroradius.

Amplification and decay depend on the direction and scale of magnetic perturbations.

Abstract

We do a detailed study on vortex formation in a magnetized plasma within the spacetime of a moving cosmic string using analytical and numerical methods. The conical spacetime around the cosmic string causes the frozen-in magnetic field to deform due to the fluid flow. We find that the overdensity in the wake region amplifies the magnetic field. This amplification depends on the direction and the lengthscale of the magnetic perturbations. Alfvens theorem of flux conservation explains this result. However, our study also shows that the magnetic field can decay depending on the perturbation lengthscale, due to the breakdown of Alfvens theorem at a certain lengthscale. This lengthscale is the gyroradius of the charged particles in the plasma. Our findings are significant for understanding magnetic reconnection in cosmic string wakes.