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

Cosmic rays can interact with the solar atmosphere and produce a slew ofsecondary messengers, making the Sun a bright gamma-ray source in the sky.Detailed observations with Fermi-LAT have shown that these interactions must bestrongly affected by solar magnetic fields in order to produce the wide rangeof observational features, such as high flux and hard spectrum. However, thedetailed mechanisms behind these features are still a mystery. In this work, wetackle this problem by performing particle-interaction simulations in the solaratmosphere in the presence of coronal magnetic fields modeled using thepotential field source surface (PFSS) model. We find that the low-energy (~GeV)gamma-ray production is significantly enhanced by the coronal magnetic fields,but the enhancement decreases rapidly with energy. The enhancement is directlycorrelated with the production of gamma rays with large deviation anglesrelative to the input cosmic-ray direction. We conclude that coronal magneticfields are essential for correctly modeling solar disk gamma rays below 10GeV,but above that the effect of coronal magnetic fields diminishes. Other magneticfield structures are needed to explain the high-energy disk emission.

Simulating gamma-ray production from cosmic rays interacting with the solar atmosphere in the presence of coronal magnetic fields