Proton aurora in the cusp during southward IMF

Average Magnetic field and Polar current System (AMPS) model values of Birkeland currents during purely northward interplanetary magnetic field for three different values of the

Due to a strong and sustained northward IMF and high solar wind pressure (for many hours) the cusp spot is seen as the ionospheric footprint of high latitude lobe reconnec- tion,

This paper discusses counterstreaming electrons, electric field turbulence, HF radar spectral width enhancements, and field-aligned currents in the southward IMF cusp

[ 35 ] During times when slow flows (<100 km/s) were observed in the plasma sheet, the solar wind electric field was on average weaker and IMF was more northward than during

An event is reported where under northward IMF and high solar wind pressure conditions, a proton spot poleward of the dayside oval and tailward of cusp recon- nection

Due to a strong and sustained northward IMF and high solar wind pressure (for many hours) the cusp spot is seen as the ionospheric footprint of high latitude lobe reconnection, giving

Sorting the data according to the location of the sunlight terminator and orientation of the interplanetary magnetic field (IMF), we find that the equivalent current resembles

"The Aurora" is challenging to reach a new genre of an image, different of those "photoreal", by symbolizing the act and giving more meaning to the animation.. It