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/

Zendy Plus

Presents the zaia usage as premium feature

ZAIA

Presents the pdf analysis as premium feature

PDF Analysis

Insights

Presents the summarisation as premium feature

Summarisation

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the access of premium content as premium feature

Premium Content

Zendy Tools

Zendy Open

We study cosmic-ray acceleration in young Type Ia Supernova Remnants (SNRs)by means of test-particle diffusive shock acceleration theory and 1-Dhydrodynamical simulations of their evolution. In addition to acceleration atthe forward shock, we explore the particle acceleration at the reverse shock inthe presence of a possible substantial magnetic field, and consequently theimpact of this acceleration on the particle spectra in the remnant. Weinvestigate the time evolution of the spectra for various time-dependentprofiles of the magnetic field in the shocked region of the remnant. We test apossible influence on particle spectra of the Alfv\'enic drift of scatteringcenters in the precursor regions of the shocks. In addition, we study theradiation spectra and morphology in a broad band from radio to gamma-rays. Itis demonstrated that the reverse shock contribution to the cosmic-ray particlepopulation of young Type Ia SNRs may be significant, modifying the spatialdistribution of particles and noticeably affecting the volume-integratedparticle spectra in young SNRs. In particular spectral structures may arise intest-particle calculations that are often discussed as signatures of non-linearcosmic-ray modification of shocks. Therefore, the spectrum and morphology ofemission, and their time evolution, differ from pure forward-shock solutions.

Particle Spectra from Acceleration at Forward and Reverse Shocks of Young Type Ia Supernova Remnants