Abstract
Abstract. Three-dimensional electromagnetic full kinetic particle code (a version of TRISTAN) is used to study the interaction of a weakly-magnetized object with a solar wind of low density. The details of two magnetospheric processes – wave activity and energetic electrons appearing at the flanks of the magnetosphere – are presented. The results of the simulation are compared with known magnetospheric data.
Highlights
Magnetospheres of magnetized objects of which we already know, result from the interaction of interplanetary plasma and electromagnetic fields with the plasma and fields existing in their vicinity
Three-dimensional, electromagnetic, full kinetic particle-in-cell (PIC) global simulations of the magnetosphere were initiated by Buneman (1993) and are being continued by Nishikawa (1997, 2001) and Cai et al (2006)
The global structure of the investigated magnetosphere of a celestial body is discussed referring to the studies of Simon et al (2006), and of Omidi et al (2002, 2003)
Summary
Magnetospheres of magnetized objects of which we already know, result from the interaction of interplanetary plasma and electromagnetic fields with the plasma and fields existing in their vicinity. Another feature of the fields excited in the region may be seen while observing the electrons. Except for two electrons, which begin their motion in the region of elevated electric field intensity (above 0.38 mV/m), the majority of the group starts in a region of weak electric field intensity – below 0.1 mV/m, with energies at a level below 1 keV
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