2014/11/25 by Z. Vörös, Y. L. Sasunov, V. S. Semenov +3
Engineering · Physics and Astronomy · #Field (mathematics) #Fluid Dynamics and Turbulent Flows #Flux (metallurgy) #Ionosphere and magnetosphere dynamics #Magnetic reconnection #Outflow #Solar and Space Plasma Dynamics #Solar wind #Turbulence #astro-ph.SR #physics.space-ph
paper · pdf · doi:10.1088/2041-8205/797/1/l10
published as The Astrophysical Journal Letters, 797: L10, 2014 · 5 figures
openalex publication_date 2014/11/25 · arxiv created 2014/11/28 · arxiv updated 2014/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Petschek-type time-dependent reconnection (TDR) and quasi-stationary reconnection (QSR) models are considered to understand reconnection outflow structures and the generation of local turbulence in the solar wind. Comparing TDR/QSR model predictions of the outflow structures with actual measurements shows that both models can explain the data equally well. It is demonstrated that the outflows can often generate more or less spatially extended turbulent boundary layers. The structure of a unique extended reconnection outflow is investigated in detail. The analysis of spectral scalings and spectral break locations shows that reconnection can change the local field and plasma conditions which may support different local turbulent dissipation mechanisms at their characteristic wavenumbers.