Energetic electron observations of Rhea’s magnetospheric interaction

Interaction of Energetic Ring Current Protons with Magnetospheric Hydromagnetic Waves

Energetic particle sounding of the magnetospheric cusp with ISEE-1

Observations on 30 October 1978 show the ISEE1 spacecraft passing though the high-altitude dayside northern magnetospheric cusp region from roughly 16:00 to 18:30 UT, during a slow solar wind period (∼380 km/s). More than two orders of magnitude enhancements of the cusp energetic particle (CEP) fluxes were observed along with a depressed and turbulent local magnetic field. The observed variatio...

STEREO and ACE Observations of Energetic Particles from Corotating Interaction Regions

Since early 2007, significant particle enhancements due to corotating interaction regions (CIRs) have regularly appeared at 1 AU without any appreciable contamination from solar energetic particles (SEPs). In 2009 the prevalence of CIRs diminished as the maximum speed of the high speed solar wind streams in the ecliptic decreased along with the tilt of the heliospheric current sheet. Observatio...

Comparative investigation of the energetic ion spectra comprising the magnetospheric ring currents of the solar system

Investigated here are factors that control the intensities and shapes of energetic ion spectra that make up the ring current populations of the strongly magnetized planets of the solar system, specifically those of Earth, Jupiter, Saturn, Uranus, and Neptune. Following a previous and similar comparative investigation of radiation belt electrons, we here turn our attention to ions. Specifically,...

Energetic Particle Observations Near the Termination Shock

The most recent data from Voyager 1 (V1) show that a second event (TS2), apparently associated with the termination shock (TS), is in progress, with spectral characteristics similar to the energetic particle increase observed from 2002.4 2003.1 (TS1) [1,2]. We concentrate on the pressure, composition, and anisotropy profiles of TS1. The magnetic field pressure [3] is significantly smaller than ...