Properties of Turbulence in the Reconnection Exhaust: Numerical Simulations Compared with Observations

被引：46

作者：

Pucci, F. ^{[1
]}

Servidio, S. ^{[2
]}

Sorriso-Valvo, L. ^{[3
]}

Olshevsky, V. ^{[1
]}

Matthaeus, W. H. ^{[4
]}

Malara, F. ^{[2
]}

Goldman, M. V. ^{[5
]}

Newman, D. L. ^{[5
]}

Lapenta, G. ^{[1
]}

机构：

[1] Katholieke Univ Leuven, Ctr Math Plasma Astrophys, Dept Wiskunde, 200B Celestijnenlaan, B-3001 Leuven, Belgium

[2] Univ Calabria, Dipartimento Fis, I-87036 Cosenza, Italy

[3] UOS Cosenza, Nanotec CNR, Via P Bucci,Cubo 31C, I-87036 Arcavacata Di Rende, Italy

[4] Univ Delaware, Dept Phys & Astron, 217 Sharp Lab, Newark, DE 19716 USA

[5] Univ Colorado, Boulder, CO 80309 USA

来源：

ASTROPHYSICAL JOURNAL | 2017年 / 841卷 / 01期

关键词：

magnetic reconnection; methods: numerical; turbulence; MAGNETIC RECONNECTION; PLASMA; POINT;

D O I：

10.3847/1538-4357/aa704f

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页数：6

共 38 条

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