Numerical simulation of oscillating magnetospheres with resistive electrodynamics

Abstract

We present a model of the magnetosphere around an oscillating neutron star. The electromagnetic fields are numerically solved by modeling electric charge and current induced by the stellar torsional mode, with particular emphasis on outgoing radiation passing through the magnetosphere. The current is modeled using Ohm's law, whereby an increase in conductivity results in an increase in the induced current. As a result, the fields are drastically modified, and energy flux is thereby enhanced. This behavior is however localized in the vicinity of the surface since the induced current disappears outwardly in our model, in which the exterior is assumed to gradually approach a vacuum.

References in corpus (7)

• The strongest cosmic magnets: Soft Gamma-ray Repeaters and Anomalous X-ray Pulsars
• Corona of Magnetars
• On the theory of magnetar QPOs
• Alfvén QPOs in Magnetars
• Magnetars oscillations in the presence of a crust
• Axisymmetric toroidal modes of magnetized neutron stars
• The Magnetosphere of Oscillating Neutron Stars in General Relativity

Cited by in corpus (6)

• Theory of pulsar magnetosphere and wind
• Magnetar Broadband X-ray Spectra Correlated with Magnetic Fields: Suzaku Archive of SGRs and AXPs Combined with NuSTAR, Swift, and RXTE
• Electromagnetic fields of slowly rotating magnetized compact stars in conformal gravity
• Modulating the magnetosphere of magnetars by internal magneto-elastic oscillations
• Axisymmetric force-free magnetosphere in the exterior of a neutron star
• Axisymmetric force-free magnetosphere in the exterior of a neutron star II: Maximum storage and open field energies