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

The origin of hard X-rays and gamma-rays emitted from the solar atmosphereduring occulted solar flares is still debated. The hard X-ray emissions couldcome from flaring loop tops rising above the limb or Coronal Mass Ejections(CME) shock waves, two by-products of energetic solar storms. For the shockscenario to work, accelerated particles must be released on magnetic fieldlines rooted on the visible disk and precipitate. We present a new Monte Carlocode that computes particle acceleration at shocks propagating along largecoronal magnetic loops. A first implementation of the model is carried out forthe 2014 September 1 event and the modeled electron spectra are compared withthose inferred from Fermi Gamma-ray Burst Monitor (GBM) measurements. Whenparticle diffusion processes are invoked our model can reproduce the hardelectron spectra measured by GBM nearly ten minutes after the estimated on-diskhard X-rays appear to have ceased from the flare site.

On the origin of hard X-ray emissions from the behind-the-limb flare on 2014 September 1