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

Energetic antiprotons in cosmic rays can serve as an important indirectsignature of dark matter. Conventionally, the antiproton flux from dark matterdecays or annihilations is calculated by solving the transport equation with aspace-independent diffusion coefficient within the diffusion zone of thegalaxy, and assuming free propagation outside this zone. Antiproton sourcesoutside of the diffusion zone are ignored. In reality, it is far more likelythat the diffusion coefficient increases smoothly with distance from the disk,and the outlying part of the dark matter halo ignored in the conventionalapproach can be significant, containing as much as 90% of the galactic darkmatter by mass in some models. We extend the conventional approach to addressthese issues. We obtain analytic approximations and numerical solutions forantiproton flux assuming that the diffusion coefficient increases exponentiallywith the distance from the disk, and including contributions from dark matterannihilations/decays in essentially the full dark matter halo. We find that theantiproton flux predicted in this model deviates from the conventionalcalculation for the same dark matter parameters by up to about 25%.

Antiprotons from Dark Matter: Effects of a Position-Dependent Diffusion Coefficient