Magnetic-field evolution with large-scale velocity circulation in a neutron-star crust
arXiv:2004.08006 · doi:10.1093/mnras/staa1045
Abstract
We examine the effects of plastic flow that appear in a neutron-star crust when a magnetic stress exceeds the threshold. The dynamics involved are described using the Navier--Stokes equation comprising the viscous-flow term, and the velocity fields for the global circulation are determined using quasi-stationary approximation. We simulate the magnetic-field evolution by taking into consideration the Hall drift, Ohmic dissipation, and fluid motion induced by the Lorentz force. The decrease in the magnetic energy is enhanced, as the energy converts to the bulk motion energy and heat. It is found that the bulk velocity induced by the Lorentz force has a significant influence in the low-viscosity and strong-magnetic-field regimes. This effect is crucial near magnetar surfaces.
References in corpus (13)
- Magnetar-like Emission from the Young Pulsar in Kes 75
- Magnetic field dissipation in neutron star crusts: from magnetars to isolated neutron stars
- A Magnetar-like Outburst from a High-B Radio Pulsar
- The Dipole Magnetic Field and Spin-down Evolutions of The High Braking Index Pulsar PSR J1640-4631
- Magnetic, thermal and rotational evolution of isolated neutron stars
- Three-dimensional simulations of the magnetic stress in a neutron star crust
- Magnetic Field Evolution of Neutron Stars I: Basic formalism, numerical techniques, and first results
- Magnetic-field evolution in a plastically-failing neutron-star crust
- NuSTAR Discovery of a Young, Energetic Pulsar Associated with the Luminous Gamma-ray Source HESS J1640-465
- Magnetic Axis Drift and Magnetic Spot Formation in Neutron Stars with Toroidal Fields
- Microscopic Vortex Velocity in the Inner Crust and Outer Core of Neutron Stars
- On the magnetic field evolution timescale in superconducting neutron star cores
- What can PSR J1640-4631 tell us about the internal physics of this neutron star?