期刊
PHYSICS OF PLASMAS
卷 16, 期 6, 页码 -出版社
AIP Publishing
DOI: 10.1063/1.3085795
关键词
astrophysical plasma; plasma simulation; plasma turbulence; solar wind
资金
- Korea Science and Engineering Foundation [R11-2008-07201003-0]
- POSCO
- Brazilian agencies Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq)
- Fundacao de Amparo Pesquisa do Estado do Rio Grande do Sul (FAPERGS)
- AFOSR [FA9550-07-0053]
The electron distributions detected in the solar wind feature varying degrees of anisotropic high-energy tail. In a recent work the present authors numerically solved the one-dimensional electrostatic weak turbulence equations by assuming that the solar wind electrons are initially composed of thermal core plus field-aligned counterstreaming beams, and demonstrated that a wide variety of asymmetric energetic tail distribution may result. In the present paper, the essential findings in this work are tested by means of full particle-in-cell simulation technique. It is found that the previous results are largely confirmed, thus providing evidence that the paradigm of local electron acceleration to high-energy tail by self-consistently excited Langmuir turbulence may be relevant to the solar wind environment under certain circumstances. However, some discrepancies are found such that the nearly one-sided energetic tail reported in the numerical solution of the weak turbulence kinetic equation is not shown.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据