Polar particle flux distribution and its spatial extent

Context: The main challenge in atmospheric ionisation modelling is that sparse measurements are used to derive a global precipitation pattern. Typically this requires intense interpolation or scaling of long-term average maps. In some regions however, the particle flux might be similar and combination these would not limit results even though it dramatically improve spatial temporal data coverage. Aims: intention paper statistically analyse distribution close geomagnetic poles labelled as Polar Particle Flux Distribution (PPFD) identify distributions neighbouring bins. Those bins grouped together size PPFD-area estimated. benefit single within should able represent for whole area at given time. Methods: We use spatially binned energetic measured by POES Metop spacecraft during 2001--2018 Kp-dependent with one found (|magn. lat|>86°). First, mapped on magnetic local time (MLT) vs. latitude grid. second step gridded split up according Kp-levels (forming final bins). Third, every bin has been recalculated order replace zero-count rates based longer measurement periods which more realistic low end distribution. Then compared PPFD. A "$\Delta$-test" indicates similarity. threshold $\Delta$-test defined using standard deviation values inside lat|>86°) area. Bins meet attributed PPFD-area. Results: Distributions corresponding PPFD-areas have determined all investigated channels, covering an energy range 154~eV--300~keV electrons 154~eV--2.5~MeV protons. Concerning channels gradual increase rising Kp identified. High show background population solar event (SPE) adds increasing Kp. depends species, disturbance, well MLT. findings are: a)~There small but characteristic hemispheric differences. b)~Only above certain energy. c)~A clear enlargement identified - exceptions very d)~The centre shifted towards midnight moves Asymmetries boundaries could explained auroral intensity. e)~For particles restriction seems precipitation.