P. C. Escoubet

Larmor radius size density holes discovered in the solar wind upstream of Earth’s bow shock

The Cluster and Double Star satellites recently observed plasma density holes upstream of Earth’s collisionless bow shock to apogee distances of ∼19 and 13 earth radii, respectively. A survey of 147 isolated density holes using 4s time resolution data shows they have a mean duration of ∼17.9±10.4s, but holes as short as 4s are observed. The average fractional density depletion (δn∕n) inside the holes is ∼0.68±0.14. The upstream edge of density holes can have enhanced densities that are five or more times the solar wind density. Particle distributions show the steepened edge can behave like a shock. Multispacecraft analyses show the density holes move with the solar wind, can have an ion gyroradius scale, and could be expanding. A small normal electric field points outward. Similarly shaped magnetic holes accompany the density holes indicating strong coupling between fields and particles. The density holes are only observed with upstream particles, suggesting that backstreaming particles interacting with t...

Identifying the source region of plasmaspheric hiss

The presence of the plasmaspheric hiss emission around the Earth has been known for more than 50 years but its origin has remained unknown in terms of source location and mechanism. The hiss, made of whistler mode waves, exists for most of the time in the plasmasphere and is believed to control the radiation belt surrounding the Earth which makes its understanding very important. This paper presents direct observational evidence that the plasmaspheric hiss originates in the equatorial region of the plasmaspheric drainage plumes. It shows that the emissions propagate along the magnetic field lines and away from the equator in the plumes but towards the equator at lower L shells inside the plasmasphere. The observations also suggest that the hiss waves inside the plasmasphere are absorbed as they cross the equator.

Density holes in the upstream solar wind

Larmor size transient structures with depletions as large as 99% of ambient solar wind density levels occur commonly upstream of Earth’s collisionless bow shock. These “density holes” have a mean duration of ∼17.9 ± 10.4s but holes as short as 4s have been observed. The average fractional density depletion (δn/n) inside the holes is ∼0.68 ± 0.14. The density of the upstream edge moving in the sunward direction can be enhanced by five or more times the solar wind density. Particle distributions show the steepened edge can behave like a shock, and measured local field geometries and Mach number support this view. Similarly shaped magnetic holes accompany the density holes indicating strong coupling between fields and particles. The density holes are only observed with upstream particles, suggesting that back‐streaming particles interacting with the solar wind are important.

Shall we carry sounders onboard future magnetospheric missions? Lessons learned from Cluster

Since 2000, the four ESA/NASA Cluster satellites orbit the Earth from 20 Re down to 1 Re. Each spacecraft is equipped with the same set of 11 plasma instruments, among which a relaxation sounder named WHISPER. Scientific highlights, where WHISPER data played a key role, will be first presented with an emphasis on plasmaspheric wave research [1]. Then, we will illustrate how WHISPER is key to estimate the electron density in various regions (sometimes unforeseen) of the magnetosphere, on its own and in conjunction with other plasma instruments [2]. These lessons learned from Cluster will help to answer the following question: shall we carry sounders onboard future magnetospheric missions?