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Related Concept Videos

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Magnetostatic Boundary Conditions

An electric field suffers a discontinuity at a surface charge. Similarly, a magnetic field is discontinuous at a surface current. The perpendicular component of a magnetic field is continuous across the interface of two magnetic mediums. In contrast, its parallel component, perpendicular to the current, is discontinuous by the amount equal to the product of the vacuum permeability and the surface current. Like the scalar potential in electrostatics, the vector potential is also continuous...
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Thermal Sigmatropic Reactions: Overview01:16

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Updated: May 26, 2026

Magnetically Induced Rotating Rayleigh-Taylor Instability
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Modified temperature-anisotropy instability thresholds in the solar wind.

R Schlickeiser1, M J Michno, D Ibscher

  • 1Institut für Theoretische Physik, Lehrstuhl IV: Weltraum- und Astrophysik, Ruhr-Universität Bochum, Germany.

Physical Review Letters
|December 21, 2011
PubMed
Summary

Collisional damping in solar wind plasma tightens constraints on temperature anisotropy instabilities. However, these refined thresholds do not fully explain observed plasma behaviors at low parallel plasma beta.

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Area of Science:

  • Plasma physics
  • Space physics
  • Astrophysics

Background:

  • Proton and electron temperature anisotropies in solar wind are limited by kinetic plasma instabilities.
  • Instability thresholds are crucial for understanding solar wind plasma behavior.

Purpose of the Study:

  • To investigate the impact of collisional damping on the instability thresholds for temperature anisotropies in solar wind plasma.
  • To refine the understanding of constraints on solar wind plasma properties.

Main Methods:

  • Calculated modifications to marginal instability conditions.
  • Accounted for damping effects from collisional processes.
  • Analyzed Alfvén waves, mirror, and firehose fluctuations.

Main Results:

  • Collisional effects introduce tighter constraints on temperature-anisotropy-driven instabilities.
  • Modified thresholds provide more stringent limits compared to marginal thresholds.
  • The refined thresholds do not completely resolve discrepancies with observations at low parallel plasma beta.

Conclusions:

  • Collisional damping plays a significant role in modulating kinetic plasma instabilities in the solar wind.
  • Existing models, even with collisional effects, may require further refinement to fully explain solar wind plasma observations, particularly at low parallel plasma beta.