Erratum: “Defining and identifying three-dimensional magnetic reconnection in resistive magnetohydrodynamic simulations of Earth’s magnetosphere” [Phys. Plasmas 15, 056504 (2008)]

2008 ◽  
Vol 15 (12) ◽  
pp. 129902
Author(s):  
John C. Dorelli ◽  
A. Bhattacharjee
Keyword(s):  
Magnetic Reconnection ◽  
Three Dimensional ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere ◽  
Magnetohydrodynamic Simulations

scholarly journals Magnetic reconnection X-line retreat associated with dipolarization of the Earth's magnetosphere

2011 ◽  
Vol 38 (20) ◽  
pp. n/a-n/a ◽  
Author(s):  
M. Oka ◽  
T.-D. Phan ◽  
J. P. Eastwood ◽  
V. Angelopoulos ◽  
N. A. Murphy ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere

scholarly journals Impacts of ionospheric ions on magnetic reconnection and Earth's magnetosphere dynamics

2021 ◽  
Author(s):  
S. Toledo‐Redondo ◽  
M. André ◽  
N. Aunai ◽  
C. R. Chappell ◽  
J. Dargent ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere

scholarly journals Solar wind interaction with the Earth's magnetosphere: the role of reconnection in the presence of a large scale sheared flow

2009 ◽  
Vol 16 (1) ◽  
pp. 1-10 ◽  
Author(s):  
F. Califano ◽  
M. Faganello ◽  
F. Pegoraro ◽  
F. Valentini
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Magnetic Reconnection ◽  
Large Scale ◽  
Initial Conditions ◽  
Magnetic Layer ◽  
Magnetic Islands ◽  
Solar Wind Interaction ◽  
Earth’S Magnetosphere ◽  
Earth's Magnetosphere

Abstract. The Earth's magnetosphere and solar wind environment is a laboratory of excellence for the study of the physics of collisionless magnetic reconnection. At low latitude magnetopause, magnetic reconnection develops as a secondary instability due to the stretching of magnetic field lines advected by large scale Kelvin-Helmholtz vortices. In particular, reconnection takes place in the sheared magnetic layer that forms between adjacent vortices during vortex pairing. The process generates magnetic islands with typical size of the order of the ion inertial length, much smaller than the MHD scale of the vortices and much larger than the electron inertial length. The process of reconnection and island formation sets up spontaneously, without any need for special boundary conditions or initial conditions, and independently of the initial in-plane magnetic field topology, whether homogeneous or sheared.

scholarly journals Magnetized Kelvin–Helmholtz instability: theory and simulations in the Earth’s magnetosphere context

2017 ◽  
Vol 83 (6) ◽  
Author(s):  
Matteo Faganello ◽  
Francesco Califano
Keyword(s):  
Three Dimensional ◽  
Solar Wind Plasma ◽  
Helmholtz Instability ◽  
Earth’S Magnetosphere ◽  
Instability Theory ◽  
Earth's Magnetosphere ◽  
Long Time ◽  
Weak Points ◽  
The Rich

The Kelvin–Helmholtz instability, proposed a long time ago for its role in and impact on the transport properties at magnetospheric flanks, has been widely investigated in the Earth’s magnetosphere context. This review covers more than fifty years of theoretical and numerical efforts in investigating the evolution of Kelvin–Helmholtz vortices and how the rich nonlinear dynamics they drive allow solar wind plasma bubbles to enter into the magnetosphere. Special care is devoted to pointing out the main advantages and weak points of the different plasma models that can be adopted for describing the collisionless magnetospheric medium and in underlying the important role of the three-dimensional geometry of the system.

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