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 Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We performed ab-initio Particle-In-Cell (PIC) simulations of a pulsarmagnetosphere with electron-positron plasma produced only in the regions closeto the neutron star surface. We study how the magnetosphere transitions fromthe vacuum to a nearly force-free configuration. We compare the resultingforce-free like configuration with ones obtained in a PIC simulation whereparticles are injected everywhere as well as with macroscopic force-freesimulations. We found that although both PIC solutions have similar structureof electromagnetic fields and current density distributions, they havedifferent particle density distribution. In fact in the injection from thesurface solution, electrons and positrons counterstream only along parts of thereturn current regions and most of the particles leave the magnetospherewithout returning to the star. We also found that pair production in the outermagnetosphere is not critical for filling the whole magnetosphere with plasma.We study how the current density distribution supporting the globalelectromagnetic configuration is formed by analyzing particle trajectories. Wefound that electrons precipitate to the return current layer inside the lightcylinder and positrons precipitate to the current sheet outside the lightcylinder by crossing magnetic field lines contributing to the charge densitydistribution required by the global electrodynamics. Moreover, there is apopulation of electrons trapped in the region close to the Y-point. On theother hand the most energetic positrons are accelerated close to the Y-point.These processes can have observational signatures that, with further modelingefforts, would help to distinguish this particular magnetosphere configurationfrom others.

Electron positron pair flow and current composition in the pulsar magnetosphere