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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

ABSTRACT  The observational determination of radiation locations can constrain pulsar radiation models. The  γ– B   process in a strong magnetic field is one of the fundamental physical processes contributing to pulsar radiation mechanisms. Photons generated near a pulsar surface with sufficient energy will be absorbed in the magnetosphere. Considering aberrational, rotational and general relativistic effects, we calculate the  γ– B   optical depth for γ‐ray photons, and we use the derived optical depth to determine the lower bounds of the radiation altitude for photons with given energies. As a case study, we obtain the low bounds of radiation altitude for the Crab pulsar for photons with energies of 5 GeV–1 TeV.

Low bounds for pulsar γ‐ray radiation altitudes