Jovian Electrons In The Inner Heliosphere: A Parameter Study On Intensity Profiles Near Earth

Abstract

Although the main processes are well known, the transport parameters of charged particles in the inner heliosphere are still under investigation. A newly developed GPU-accelerated code to solve Parker's transport equation by means of stochastic differential equations (SDEs) offers the possibility to perform extensive parameter studies. Investigating electrons originating from the Jovian magnetosphere, we will present the potential of the code as well as first results of the time profile near Earth as a function of varying the solar wind speed, the strength of the diffusion and relation between the parallel and the perpendicular diffusion coefficient.

Cosmic-Ray Transport in Heliospheric Magnetic Structures. II. Modeling Particle Transport through Corotating Interaction Regions

“…In particular, it is necessary to first propagate the Local Interstellar Spectrum (LIS) at the heliopause (see the right panel in Figure 1) inwardand then to provide the resulting CR spectrum as a boundary condition for particles leaving the heliosphere. Aside from the technical realization, an artificially close boundary leads to an incorrect solution of the transport equation as demonstrated for the case of Jovian electrons by Vogt et al (2015). In the present study we thus treaded another path, visualized by zooming into the simulation region in the left and middle panels of Figure 1: the distance of the outer boundary and the LIS are kept at the quantities given below.…”