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Magnetically Induced Rotating Rayleigh-Taylor Instability
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Thin-shell instability in collisionless plasma.

M E Dieckmann1, H Ahmed2, D Doria2

  • 1Department of Science and Technology, Linköping University, SE-60174 Norrköping, Sweden.

Physical Review. E, Statistical, Nonlinear, and Soft Matter Physics
|October 15, 2015
PubMed
Summary
This summary is machine-generated.

Thin-shell instability can create complex structures in astrophysical plasma. Particle-in-cell simulations show this instability can disrupt thin shells formed by colliding plasma clouds, leading to spatial modulations.

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Area of Science:

  • Plasma Physics
  • Astrophysical Plasmas
  • Computational Astrophysics

Background:

  • Thin-shell instability is a known mechanism for generating entangled structures in collisional astrophysical plasmas.
  • This instability arises from pressure imbalances at nonplanar shocks.
  • Understanding such instabilities is crucial for modeling astrophysical phenomena.

Purpose of the Study:

  • To investigate if a similar instability affects thin shells in collisionless plasmas.
  • To explore the dynamics of thin shells formed by interpenetrating plasma clouds using simulations.

Main Methods:

  • Particle-in-cell (PIC) simulations were employed.
  • The study focused on two interpenetrating, unmagnetized, and collisionless plasma clouds.
  • Simulation parameters were analyzed over time, specifically in relation to proton plasma frequencies.

Main Results:

  • An analog of thin-shell instability was observed in collisionless plasma shells.
  • The spatial modulation amplitude of the shell grew significantly.
  • The instability saturated after approximately ten inverse proton plasma frequencies, forming piecewise linear structures.

Conclusions:

  • Thin-shell instability is not limited to collisional plasmas and can occur in collisionless systems.
  • Interpenetrating plasma clouds can form unstable thin shells that evolve into complex, modulated structures.
  • The findings provide insights into structure formation in astrophysical environments.