Open Access
Research Article
Issue
J. Space Weather Space Clim.
Volume 10, 2020
Article Number 51
Number of page(s) 17
DOI https://doi.org/10.1051/swsc/2020053
Published online 14 October 2020

Suplementary Materials

The Supporting Information consists of four animations numbered S1–S4, whose descriptions are given below.

Animation S1

Animation of the proton temperature in a zoomed-in box centred on the dayside magnetosphere in the southward IMF simulation. The two locations in the northern and southern cusps where the precipitating fluxes can be derived at each time step are shown with black circles, and the inset axes show cuts of the corresponding VDFs in the (vx, vz) frame, with the loss cone indicated in magenta (northern cusp VDF) or brown (southern cusp VDF). The black lines represent magnetic field lines. The velocity grid spacing is 1000 km/s. The animation starts at t = 1350 s and lasts until the end of the simulation at t = 2150 s, with one frame every 0.5 s. (IMF: interplanetary magnetic field; VDF: velocity distribution function).

Animation S2

Animation of the proton temperature in a zoomed-in box centred on the dayside magnetosphere in the northward IMF simulation. The five locations shown with black circles indicate the cells where the precipitating fluxes are calculated, and the inset axes show cuts of the corresponding VDFs in the (vx, vz) frame, with the loss cone indicated in magenta and brown for precipitation in the northern and southern cusps, respectively. The black lines represent magnetic field lines. The velocity grid spacing is 1000 km/s. The animation starts at t = 1100 s and lasts until the end of the simulation at t = 1938 s, with one frame every 0.5 s. (IMF: interplanetary magnetic field; VDF: velocity distribution function).

Animation S3

Animation of the y (dawn/dusk) component of the magnetic field in a zoomed-in box centred on the dayside magnetosphere in the northward IMF simulation. The five locations shown with black circles indicate the cells where the precipitating fluxes are calculated, and the inset axes show cuts of the corresponding VDFs in the (vx, vz) frame, with the loss cone indicated in magenta and brown for precipitation in the northern and southern cusps, respectively. The black lines represent magnetic field lines. The velocity grid spacing is 1000 km/s. The animation starts at t = 1100 s and lasts until the end of the simulation at t = 1938 s, with one frame every 0.5 s. (IMF: interplanetary magnetic field; VDF: velocity distribution function).

Animation S4

Animation of the y (dawn/dusk) component of the magnetic field in a zoomed-in box centred on the dayside magnetosphere in the southward IMF simulation. The two locations in the northern and southern cusps where the precipitating fluxes can be derived at each time step are shown with black circles, and the inset axes show cuts of the corresponding VDFs in the (vx, vz) frame, with the loss cone indicated in magenta (northern cusp VDF) or brown (southern cusp VDF). The black lines represent magnetic field lines. The velocity grid spacing is 1000 km/s. The animation starts at t = 1350 s and lasts until the end of the simulation at t = 2150 s, with one frame every 0.5 s. (IMF: interplanetary magnetic field; VDF: velocity distribution function).

© M. Grandin et al., Published by EDP Sciences 2020