Journal of Geophysical Research: Space Physics

Plasma density normalized to solar wind value at four times (proton gyroperiods Ω–1) demonstrating the interaction of SHFA with the bow shock.

Three-dimensional plot of solar wind interaction with Venus for solar max case, with the left panel showing an upstream view, while the right panel a downstream view. The white lines with arrows are magnetic field lines. The gray isosurface represents a density contour with planetary O+ density equals to 100 cm–3 as an indication of Venus ionopause.

Pictures taken by CEO where sprites are obviously detected. The different point of views of CEO observations (oblique and toward the limb) clearly appear in the images as well as typical nighttime observations: stars, ionospheric layers, auroras, towns, lightning flashes, sprites (identified with a letter printed close to them), and the ISS itself.

Images of the plasmasphere obtained by the EUV imager on board the IMAGE satellite during the geomagnetic storm of 21 October 2001. In each panel, the view is of the SM-coordinate magnetic equatorial plane, with the Earth in the center and the Sun to the right. The faint dotted white circle is geostationary orbit. The red dots indicate locations of the plasmapause inferred from these images. High background counts outside the plasmapause and partial loss of the dayside signal from sunlight contamination are nonphysical/instrumental.

The Z (a transverse) component of the magnetic field from 4 runs with O+ ion density of 0%, 7%, 15%, and 30% of the cold background protons.