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

We investigate the influence of magneticmirroring and elastic and inelastic scattering on the angular redistribution ina proton/hydrogen beam by using a transport code in comparison withobservations. H-emission Doppler profiles viewed in the magnetic zenith exhibita red-shifted component which is indicative of upward fluxes. In order todetermine the origin of this red shift, we evaluate the influence of two angularredistribution sources which are included in our proton/hydrogen transportmodel. Even though it generates an upward flux, the redistribution due tomagnetic mirroring effect is not sufficient to explain the red shift. On theother hand, the collisional angular scattering induces a much more significantred shift in the lower atmosphere. The red shift due to collisions isproduced  by <1 -keV protons and is so small as to require an instrumental bandwidth<0.2 nm. This explains the absence of measured upward proton/hydrogen fluxesin the Proton I rocket data because no useable data concerning protons <1 keVare available. At the same time, our model agrees with measured ground-basedH-emission Doppler profiles and suggests that previously reported red shiftobservations were due mostly to instrumental bandwidth broadening of theprofile. Our results suggest that Doppler profile measurements with higherspectral resolution may enable us to quantify better the angular scattering inproton aurora.  <b>Key words.</b> Auroral ionosphere · Particle precipitatio

Proton transport model in the ionosphere. 2. Influence of magnetic mirroring and collisions on the angular redistribution in a proton beam