Search arXiv⌕ Search

arXiv · astro-ph/0502477

Nonlinear Perpendicular Diffusion in Strong Turbulent Electromagnetic Fields

Abstract

A nonlinear description for perpendicular particle diffusion in strong electromagnetic fluctuations is developed by using the fundamental Newton-Lorentz equation. Although not based on the same approach, the recently presented nonlinear guiding center (NLGC) theory is recovered as a special case. The approach used here is rather based on the argument that a well defined particle gyromotion does not exist in strong fluctuations than on the assumption that the particle gyrocenter follows magnetic field lines which themselves separate diffusively. The assumption of a guiding center motion and the diffusive separation of magnetic field lines is absolutely central to the NLGC theory. It is argued that the NLGC result should provide most accurate results for strong fluctuations. Furthermore, as a direct consequence of the particle equation of motion, it is shown that particle diffusion in one perpendicular direction is governed by the fluctuations in the other normal direction. This results contradicts the NLGC result, where perpendicular diffusion is triggered by fluctuations in the same direction. This is of particular interest for anisotropic perpendicular diffusion in a non-axisymmetric turbulence. Future numerical simulation results for non-axisymmetric magnetic turbulence and their comparison with the approach presented here and the NLGC theory have to provide an answer whether particle diffusion in one perpendicular direction is governed by the fluctuations in the other normal direction or by fluctuations in the same direction.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

O. Stawicki. 2005-02-23. Nonlinear Perpendicular Diffusion in Strong Turbulent Electromagnetic Fields. https://doi.org/10.1016/j.asr.2005.02.008

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

Cosmic Conundrums with Quantum Corrections

Darh energy was discovered over 25 years ago and we do not have an explanation of it. Dark matter comprises 95% of matter in the universe and we still don't know what it is. The Webb telescope has been finding fully formed galaxies with massive black holes millions of times the mass of the sun in the early universe and we don't have any explanation. A quantum density limitation will be used to solve these and other outstanding problems.

astro-ph↗

On binary pulsars and the force of gravity

The energy-momentum budget of the astrophysical systems can be studied by the exact local conservation equation derived by Landau and Lifshitz. We show that a similar equation is valid for the Einstein-Cartan gravity. We reanalyze a binary pulsar system using the Landau-Lifshitz conservation equation and show that the orbital period change rate can be completely understood as a curvature backreaction process. Taking into account the detailed theoretical and observational research of relativistic binary pulsar systems, especially the system of Hulse and Taylor, we conclude that general relativity and astrophysical observations rule out the existence of gravitational radiation. We comment upon the LIGO GW events and their alternative explanation, as well as the recent pulsar timing arrays data.

astro-ph↗

Oscillation frequencies and mode lifetimes in alpha Centauri A

We analyse our recently-published velocity measurements of alpha Cen A (Butler et al. 2004). After adjusting the weights on a night-by-night basis in order to optimize the window function to minimize sidelobes, we extract 42 oscillation frequencies with l=0 to 3 and measure the large and small frequency separations. We give fitted relations to these frequencies that can be compared with theoretical models and conclude that the observed scatter about these fits is due to the finite lifetimes of the oscillation modes. We estimate the mode lifetimes to be 1-2 d, substantially shorter than in the Sun.

astro-ph↗