Statistical Characteristics in the Spectrum of Whistler Waves near the Diffusion Region of dayside Magnetopause Reconnection

2020 ◽  
Author(s):  
Y. Ren ◽  
L. Dai ◽  
C.Wang ◽  
W. Li ◽  
X. Tao ◽  
...  
Keyword(s):  
Statistical Characteristics ◽  
Diffusion Region ◽  
Whistler Waves ◽  
Dayside Magnetopause ◽  
Magnetopause Reconnection

Observations of Whistler Waves in the Magnetic Reconnection Diffusion Region

2018 ◽  
Author(s):  
S. Y. Huang ◽  
Z. G. Yuan ◽  
H. S. Fu ◽  
A. Vaivads ◽  
F. Sahraoui ◽  
...  
Keyword(s):  
Magnetic Reconnection ◽  
Diffusion Region ◽  
Whistler Waves

Hybrid-Vlasov modelling of three-dimensional dayside magnetopause reconnection

2021 ◽  
Author(s):  
Yann Pfau-Kempf ◽  
Minna Palmroth ◽  
Andreas Johlander ◽  
Lucile Turc ◽  
Markku Alho ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Magnetic Reconnection ◽  
Three Dimensional ◽  
Meridional Plane ◽  
Kinetic Behavior ◽  
Dayside Magnetopause ◽  
Field Junction ◽  
First Time ◽  
Kinetic Instabilities ◽  
Magnetopause Reconnection

<p>Dayside magnetic reconnection at the magnetopause, which is a major driver of space weather, is studied for the first time in a three-dimensional (3D) realistic setup using the Vlasiator hybrid-Vlasov kinetic model. A noon–midnight meridional plane simulation is extended in the dawn–dusk direction to cover 7 Earth radii. The southward interplanetary magnetic field causes magnetic reconnection to occur at the subsolar magnetopause. Perturbations arising from kinetic instabilities in the magnetosheath appear to modulate the reconnection. Its characteristics are consistent with multiple, bursty, and patchy magnetopause reconnection. It is shown that the kinetic behavior of the plasma, as simulated by the model, has consequences on the applicability of methods such as the four-field junction to identify and analyse magnetic reconnection in 3D kinetic simulations.</p>

scholarly journals A numerical model of the ionospheric signatures of time-varying magnetic reconnection: III. Quasi-instantaneous convection responses in the Cowley-Lockwood paradigm

2006 ◽  
Vol 24 (3) ◽  
pp. 961-972 ◽  
Author(s):  
S. K. Morley ◽  
M. Lockwood
Keyword(s):  
The Other ◽  
Closed Field ◽  
Time Varying ◽  
Residual Flow ◽  
Numerical Implementation ◽  
Ionospheric Convection ◽  
Dayside Magnetopause ◽  
History Of ◽  
Closed Field Line ◽  
Magnetopause Reconnection

Abstract. Using a numerical implementation of the cowlock92 model of flow excitation in the magnetosphere-ionosphere (MI) system, we show that both an expanding (on a ~12-min timescale) and a quasi-instantaneous response in ionospheric convection to the onset of magnetopause reconnection can be accommodated by the Cowley-Lockwood conceptual framework. This model has a key feature of time dependence, necessarily considering the history of the coupled MI system. We show that a residual flow, driven by prior magnetopause reconnection, can produce a quasi-instantaneous global ionospheric convection response; perturbations from an equilibrium state may also be present from tail reconnection, which will superpose constructively to give a similar effect. On the other hand, when the MI system is relatively free of pre-existing flow, we can most clearly see the expanding nature of the response. As the open-closed field line boundary will frequently be in motion from such prior reconnection (both at the dayside magnetopause and in the cross-tail current sheet), it is expected that there will usually be some level of combined response to dayside reconnection.

scholarly journals Dayside Magnetopause Reconnection: Its Dependence on Solar Wind and Magnetosheath Conditions

2019 ◽  
Vol 124 (11) ◽  
pp. 8778-8787
Author(s):  
D. Koga ◽  
W. D. Gonzalez ◽  
V. M. Souza ◽  
F. R. Cardoso ◽  
C. Wang ◽  
...  
Keyword(s):  
Solar Wind ◽  
Dayside Magnetopause ◽  
Magnetopause Reconnection

Electron‐Scale Magnetic Structure Observed Adjacent to an Electron Diffusion Region at the Dayside Magnetopause

2019 ◽  
Vol 124 (12) ◽  
pp. 10153-10169
Author(s):  
S. Hoilijoki ◽  
R. E. Ergun ◽  
S. J. Schwartz ◽  
S. Eriksson ◽  
F. D. Wilder ◽  
...  
Keyword(s):  
Magnetic Structure ◽  
Diffusion Region ◽  
Electron Diffusion ◽  
Dayside Magnetopause

scholarly journals Locating dayside magnetopause reconnection with exhaust ion distributions

2017 ◽  
Vol 122 (5) ◽  
pp. 5105-5113 ◽  
Author(s):  
J. M. Broll ◽  
S. A. Fuselier ◽  
K. J. Trattner
Keyword(s):  
Ion Distributions ◽  
Dayside Magnetopause ◽  
Magnetopause Reconnection

scholarly journals Ion-scale structure in Mercury's magnetopause reconnection diffusion region

2016 ◽  
Vol 43 (12) ◽  
pp. 5935-5942 ◽  
Author(s):  
Daniel J. Gershman ◽  
John C. Dorelli ◽  
Gina A. DiBraccio ◽  
Jim M. Raines ◽  
James A. Slavin ◽  
...  
Keyword(s):  
Scale Structure ◽  
Diffusion Region ◽  
Magnetopause Reconnection

scholarly journals Evidence for transient, local ion foreshocks caused by dayside magnetopause reconnection

2016 ◽  
Vol 34 (11) ◽  
pp. 943-959 ◽  
Author(s):  
Yann Pfau-Kempf ◽  
Heli Hietala ◽  
Steve E. Milan ◽  
Liisa Juusola ◽  
Sanni Hoilijoki ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Interplanetary Magnetic Field ◽  
Ion Beams ◽  
Bow Shock ◽  
Flux Transfer Events ◽  
Dayside Magnetopause ◽  
Flux Transfer ◽  
Push Out ◽  
Magnetopause Reconnection

Abstract. We present a scenario resulting in time-dependent behaviour of the bow shock and transient, local ion reflection under unchanging solar wind conditions. Dayside magnetopause reconnection produces flux transfer events driving fast-mode wave fronts in the magnetosheath. These fronts push out the bow shock surface due to their increased downstream pressure. The resulting bow shock deformations lead to a configuration favourable to localized ion reflection and thus the formation of transient, travelling foreshock-like field-aligned ion beams. This is identified in two-dimensional global magnetospheric hybrid-Vlasov simulations of the Earth's magnetosphere performed using the Vlasiator model (http://vlasiator.fmi.fi). We also present observational data showing the occurrence of dayside reconnection and flux transfer events at the same time as Geotail observations of transient foreshock-like field-aligned ion beams. The spacecraft is located well upstream of the foreshock edge and the bow shock, during a steady southward interplanetary magnetic field and in the absence of any solar wind or interplanetary magnetic field perturbations. This indicates the formation of such localized ion foreshocks.

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