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      A generalized two-component model of solar wind turbulence and ab initio diffusion mean free paths and drift lengthscales of cosmic rays

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          Abstract

          We extend a two-component model for the evolution of fluctuations in the solar wind plasma so that it is fully three-dimensional (3D) and also coupled self-consistently to the large-scale magnetohydrodynamic (MHD) equations describing the background solar wind. The two classes of fluctuations considered are a high-frequency parallel-propagating wave-like piece and a low-frequency quasi-two-dimensional component. For both components, the nonlinear dynamics is dominanted by quasi-perpendicular spectral cascades of energy. Driving of the fluctuations, by, for example, velocity shear and pickup ions, is included. Numerical solutions to the new model are obtained using the Cronos framework, and validated against previous simpler models. Comparing results from the new model with spacecraft measurements, we find improved agreement relative to earlier models that employ prescribed background solar wind fields. Finally, the new results for the wave-like and quasi-two-dimensional fluctuations are used to calculate ab initio diffusion mean free paths and drift lengthscales for the transport of cosmic rays in the turbulent solar wind.

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          Author and article information

          Journal
          2016-09-27
          Article
          1609.08271
          2b6398de-8420-4d76-995d-44be3593be80

          http://arxiv.org/licenses/nonexclusive-distrib/1.0/

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          Custom metadata
          ApJ, accepted
          astro-ph.SR physics.space-ph

          Space Physics,Solar & Stellar astrophysics
          Space Physics, Solar & Stellar astrophysics

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