A study of the compatibility between observations and model simulations for Jovian and galactic electrons

作     者：Ferreira, SES Potgieter, MS Heber, B Fichtner, H Burger, RA Ferrando, P 

作者机构：Potchefstroom Univ Christian Higher Educ Unit Space Phys Sch Phys ZA-2520 Potchefstroom South Africa Ruhr Univ Bochum Inst Theoret Phys 4 D-4630 Bochum Germany Max Planck Inst Aeron Katlenburg Duhm Germany CEA Saclay DAPNIA Serv Astrophys F-91191 Gif Sur Yvette France 

出 版 物：《GALACTIC AND ANOMALOUS COSMIC RAYS IN THE HELIOSPHERE: THE CYCLE 22 SOLAR MINIMUM AND THE ONSET OF CYCLE 23》 (空间研究进展)

年 卷 期：2001年第27卷第3期

页      面：553-558页

核心收录：

学科分类：08[工学] 0708[理学-地球物理学] 0706[理学-大气科学] 0704[理学-天文学] 0825[工学-航空宇航科学与技术] 

主　　题：Electron fluxes Numerical simulations Galactic models Galaxies Jupiter Ulysses spacecraft Diffusion coefficient Galactic electrons 

摘      要：The heliospheric modulation of galactic and Jovian electrons is studied using a newly developed complete three-dimensional, steady-state model based on Parker s transport equation including a Jovian source. The modulation of low-energy electrons is a handy tool to establish and to construct a suitable diffusion tensor to assure compatibility between model computations and observations from the Ulysses, Voyager and Pioneer spacecraft. Electrons respond, e.g., directly to the energy dependence of the diffusion coefficients below similar to 500 MeV in contrast to protons which experience large adiabatic energy losses below this energy. The model is used to illustrate how the low-energy electron intensities are affected at different latitudes when enhancing perpendicular diffusion in the polar direction. In particular, the electron intensity-time-profile along the Ulysses trajectory is calculated for various diffusion coefficients and compared to the 3 - 10 MeV electron flux observed by Ulysses. The results show how the relative contribution of low-energy galactic and Jovian electrons vary with respect to the total electron intensity for the various diffusion coefficients. (C) 2001 COSPAR. Published by Elsevier Science Ltd. All rights reserved.