A Measurement of the Effective Mean-Free-Path of Solar Wind Protons

Abstract

Weakly collisional plasmas are subject to nonlinear relaxation processes, which can operate at rates much faster than the particle collision frequencies. This causes the plasma to respond like a magnetised fluid despite having long particle mean-free-paths. In this Letter the effective collisional mechanisms are modelled in the plasma kinetic equation to produce density, pressure and magnetic field responses to compare with spacecraft measurements of the solar wind compressive fluctuations at 1 AU. This enables a measurement of the effective mean-free-path of the solar wind protons, found to be 4.35 $\times 10^5$ km, which is $\sim 10^3$ times shorter than the collisional mean-free-path. These measurements are shown to support the effective fluid behavior of the solar wind at scales above the proton gyroradius and demonstrate that effective collision processes alter the thermodynamics and transport of weakly collisional plasmas.

References in corpus (4)

• Recent progress in astrophysical plasma turbulence from solar wind observations
• Magnetorotational Turbulence and Dynamo in a Collisionless Plasma
• Suppressed effective viscosity in the bulk intergalactic plasma
• Constraints on dynamo action in plasmas

Cited by in corpus (4)

• The polytropic behavior of Solar Wind protons as observed by Ulysses spacecraft during Solar minimum
• The structure of 3D collisional magnetized bow shocks in pulsed-power-driven plasma flow
• Temperature anisotropy instabilities driven by intermittent velocity shears in the solar wind
• Transport of electrons in tangled magnetic fields