Properties of Turbulence in the Reconnection Exhaust: Numerical Simulations Compared with Observations
- Center for Mathematical Plasma Astrophysics, Department Wiskunde, KU Leuven, 200B Celestijnenlaan, Leuven, B-3001 (Belgium)
- Dipartimento di Fisica, Università della Calabria, I-87036 Cosenza (Italy)
- Nanotec-CNR, U.O.S. di Cosenza, Via P. Bucci, Cubo 31C, Arcavacata di Rende, I-87036 (Italy)
- Department of Physics and Astronomy, University of Delaware, 217 Sharp Lab, Newark, DE 19716 (United States)
The properties of the turbulence that develops in the outflows of magnetic reconnection have been investigated using self-consistent plasma simulations, in three dimensions. As commonly observed in space plasmas, magnetic reconnection is characterized by the presence of turbulence. Here we provide a direct comparison of our simulations with reported observations of reconnection events in the magnetotail, investigating the properties of the electromagnetic field and the energy conversion mechanisms. In particular, simulations show the development of a turbulent cascade consistent with spacecraft observations, statistics of the dissipation mechanisms in the turbulent outflows similar to the ones observed in reconnection jets in the magnetotail, and that the properties of turbulence vary as a function of the distance from the reconnecting X-line.
- OSTI ID:
- 22663573
- Journal Information:
- Astrophysical Journal, Vol. 841, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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