Abstract
A simple point of view that non-zero Alfvén ratio (residual energy) appears as a consequence of one-fluid modeling of uni-directional Alfvén waves in a solar wind plasma is presented. Since relative speeds among ions are incorporated into the one-fluid model as a pressure anisotropy, the Alfvén ratio can be finite due to the decrease in the phase velocity. It is shown that a proton beam component typically found in the solar wind plasma can contribute to generating non-zero Alfvén ratio observed in the solar wind plasma. Local equilibrium velocity distribution functions of each ion component are also discussed by using maximum entropy principle.
Original language | English |
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Article number | 124502 |
Journal | Physics of Plasmas |
Volume | 22 |
Issue number | 12 |
DOIs | |
State | Published - 2015/12/01 |
ASJC Scopus subject areas
- Condensed Matter Physics