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Title: RECONNECTION OUTFLOW GENERATED TURBULENCE IN THE SOLAR WIND

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.
Authors:
; ; ;  [1] ;  [2] ;  [3]
  1. Austrian Academy of Sciences, Space Research Institute, A-8042 Graz (Austria)
  2. Physical Institute, Saint Petersburg State University, St. Petersburg (Russian Federation)
  3. INAF-IAPS, Istituto di Astrofisica e Planetologia Spaziali, I-00133 Rome (Italy)
Publication Date:
OSTI Identifier:
22364874
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 797; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; COMPARATIVE EVALUATIONS; MAGNETIC FIELDS; MAGNETIC RECONNECTION; PLASMA; SOLAR WIND; STAR MODELS; TIME DEPENDENCE; TURBULENCE