Electron and proton heating by solar wind turbulence

被引：96

作者：

Breech, B. ^{[1
]}

Matthaeus, W. H. ^{[2
,3
]}

Cranmer, S. R. ^{[4
]}

Kasper, J. C. ^{[4
]}

Oughton, S. ^{[5
]}

机构：

[1] NASA, Goddard Space Flight Ctr, Lab Solar & Space Phys, Greenbelt, MD 20716 USA

[2] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA

[3] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA

[4] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[5] Univ Waikato, Dept Math, Hamilton 3240, New Zealand

来源：

JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS | 2009年 / 114卷

基金：

美国国家航空航天局;

关键词：

ALFVENIC TURBULENCE; SPATIAL TRANSPORT; DISSIPATION; EVOLUTION; WAVES; FLUX; 1-AU;

D O I：

10.1029/2009JA014354

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Previous formulations of heating and transport associated with strong magnetohydrodynamic (MHD) turbulence are generalized to incorporate separate internal energy equations for electrons and protons. Electron heat conduction is included. Energy is supplied by turbulent heating that affects both electrons and protons and is exchanged between them via collisions. Comparison to available Ulysses data shows that a reasonable accounting for the data is provided when (1) the energy exchange timescale is very long and (2) the deposition of heat due to turbulence is divided, with 60% going to proton heating and 40% into electron heating. Heat conduction, determined here by an empirical fit, plays a major role in describing the electron data.

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