TURBULENCE AND PROTON-ELECTRON HEATING IN KINETIC PLASMA

被引:46
作者
Matthaeus, William H. [1 ]
Parashar, Tulasi N. [1 ]
Wan, Minping [2 ]
Wu, P. [1 ]
机构
[1] Univ Delaware, Dept Phys & Astron, Bartol Res Inst, Newark, DE 19716 USA
[2] South Univ Sci & Technol China, Dept Mech & Aerosp Engn, Shenzhen 518055, Guangdong, Peoples R China
基金
美国国家科学基金会;
关键词
galaxies: ISM; ISM: kinematics and dynamics; plasmas; solar-terrestrial relations; solar wind; turbulence; TEST-PARTICLE-ACCELERATION; SOLAR-WIND TURBULENCE; MAGNETOHYDRODYNAMIC TURBULENCE; MAGNETIC-FIELD; DISSIPATION RANGE; RECONNECTION; SIMULATIONS; CASCADE;
D O I
10.3847/2041-8205/827/1/L7
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Analysis of particle-in-cell simulations of kinetic plasma turbulence reveals a connection between the strength of cascade, the total heating rate, and the partitioning of dissipated energy into proton heating and electron heating. A von Karman scaling of the cascade rate explains the total heating across several families of simulations. The proton to electron heating ratio increases in proportion to total heating. We argue that the ratio of gyroperiod to nonlinear turnover time at the ion kinetic scales controls the ratio of proton and electron heating. The proposed scaling is consistent with simulations.
引用
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页数:5
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