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

Magnetars are comparatively young neutron stars with ultra-strong surfacemagnetic field in the range $10^{14-16}$ G. The old neutron stars have surfacemagnetic field some what less $\sim 10^8$ G which clearly indicates the decayof field with time. One possible way of magnetic field decay is by ambipolardiffusion. We describe the general procedure to solve for the ambipolarvelocity inside the star core without any approximation. With a realistic modelof neutron star we determine the ambipolar velocity configuration inside theneutron star core and hence find the ambipolar decay rate and time scale whichis consistent with the magnetar observations.

Ambipolar decay of magnetic field in magnetars and the observed magnetar activities