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Solar-wind proton anisotropy versus beta relation.

Jungjoon Seough1, Peter H Yoon1, Khan-Hyuk Kim1

  • 1School of Space Research, Kyung Hee University, Yongin, Gyeonggi 446-701, Korea.

Physical Review Letters
|August 29, 2014
PubMed
Summary
This summary is machine-generated.

Solar wind proton temperature anisotropy is explained by mirror and oblique fire-hose instabilities. These instabilities regulate proton temperatures in the solar wind, matching observational data near Earth.

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Area of Science:

  • Space Physics
  • Plasma Physics
  • Astrophysics

Background:

  • Proton temperature anisotropy in the solar wind is a persistent puzzle.
  • Instabilities like mirror and oblique fire-hose are suspected regulators.
  • Previous models did not fully account for dynamic magnetic field variations.

Purpose of the Study:

  • To propose a mechanism explaining proton temperature anisotropy regulation.
  • To investigate the role of time-varying magnetic fields in instability saturation.
  • To analyze the influence of initial conditions on instability dynamics.

Main Methods:

  • Quasilinear analysis of plasma instabilities.
  • Inclusion of intermediate-scale temporal variations in the local magnetic field.
  • Modeling with arbitrary initial temperature ratios and parallel betas.

Main Results:

  • Saturated states in (parallel beta, perpendicular-to-parallel temperature ratio) space are bounded.
  • The boundaries are defined by the mirror and oblique fire-hose instabilities.
  • The model's predictions align with observed proton temperature anisotropy.

Conclusions:

  • Time-varying magnetic fields provide a viable explanation for observed proton temperature anisotropy.
  • Mirror and oblique fire-hose instabilities play a crucial role in regulating solar wind plasma.
  • The findings offer a new perspective on plasma behavior in the near-Earth solar wind.