English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Magnetospheres of many astrophysical objects can be accurately described bythe low-inertia (or "force-free") limit of MHD. We present a new numericalmethod for solution of equations of force-free relativistic MHD based on thefinite-difference time-domain (FDTD) approach with a prescription for handlingspontaneous formation of current sheets. We use this method to study thetime-dependent evolution of pulsar magnetospheres in both aligned and obliquemagnetic geometries. For the aligned rotator we confirm the general propertiesof the time-independent solution of Contopoulos et al. (1999). For the obliquerotator we present the 3D structure of the magnetosphere and compute, for thefirst time, the spindown power of pulsars as a function of inclination of themagnetic axis. We find the pulsar spindown luminosity to be L = (mu^2Omega^4/c^3) (1+ sin^2(alpha)) for a star with the dipole moment "mu", rotationfrequency "Omega", and magnetic inclination angle "alpha". We also discuss theeffects of current sheet resistivity and reconnection on the structure andevolution of the magnetosphere.

Time-dependent Force-free Pulsar Magnetospheres: Axisymmetric and Oblique Rotators