Generation mechanisms for magnetosphere-ionosphere current systems deduced from a three-dimensional MHD simulation of the solar wind-magnetosphere-ionosphere coupling processes

1995 ◽  
Vol 100 (A7) ◽  
pp. 12057 ◽  
Author(s):  
T. Tanaka
Keyword(s):  
Solar Wind ◽  
Three Dimensional ◽  
Mhd Simulation ◽  
Generation Mechanisms ◽  
Coupling Processes ◽  
Current Systems

scholarly journals Full compressible 3D MHD simulation of solar wind

2020 ◽  
Vol 500 (4) ◽  
pp. 4779-4787
Author(s):  
Takuma Matsumoto
Keyword(s):  
Solar Wind ◽  
Transition Region ◽  
Solar Physics ◽  
Mass Loss Rate ◽  
Three Dimensional ◽  
Lower Atmosphere ◽  
Fast Solar Wind ◽  
Solar Mass ◽  
Mhd Simulation ◽  
Driving Mechanisms

ABSTRACT Identifying the heating mechanisms of the solar corona and the driving mechanisms of solar wind are key challenges in understanding solar physics. A full three-dimensional compressible magnetohydrodynamic (MHD) simulation was conducted to distinguish between the heating mechanisms in the fast solar wind above the open field region. Our simulation describes the evolution of the Alfvénic waves, which includes the compressible effects from the photosphere to the heliospheric distance s of 27 solar radii (R⊙). The hot corona and fast solar wind were reproduced simultaneously due to the dissipation of the Alfvén waves. The inclusion of the transition region and lower atmosphere enabled us to derive the solar mass-loss rate for the first time by performing a full three-dimensional compressible MHD simulation. The Alfvén turbulence was determined to be the dominant heating mechanism in the solar wind acceleration region (s > 1.3 R⊙), as suggested by previous solar wind models. In addition, shock formation and phase mixing are important below the lower transition region (s < 1.03 R⊙) as well.

A three-dimensional MHD simulation of the interaction of the solar wind with comet Halley

1988 ◽  
Vol 93 (A9) ◽  
pp. 9568 ◽  
Author(s):  
Tatsuki Ogino ◽  
Raymond J. Walker ◽  
Maha Ashour-Abdalla
Keyword(s):  
Solar Wind ◽  
Three Dimensional ◽  
Mhd Simulation ◽  
Comet Halley

scholarly journals Multiple transpolar auroral arcs reveal insight about coupling processes in the Earth’s magnetotail

2020 ◽  
Vol 117 (28) ◽  
pp. 16193-16198
Author(s):  
Qing-He Zhang ◽  
Yong-Liang Zhang ◽  
Chi Wang ◽  
Michael Lockwood ◽  
Hui-Gen Yang ◽  
...  
Keyword(s):  
Solar Wind ◽  
Three Dimensional ◽  
Formation Mechanisms ◽  
Solar Wind Flow ◽  
High Latitude Ionosphere ◽  
Magnetospheric Boundary ◽  
Energy And Momentum ◽  
Magnetosphere Plasma ◽  
Auroral Arcs ◽  
Coupling Processes

A distinct class of aurora, called transpolar auroral arc (TPA) (in some cases called “theta” aurora), appears in the extremely high-latitude ionosphere of the Earth when interplanetary magnetic field (IMF) is northward. The formation and evolution of TPA offers clues about processes transferring energy and momentum from the solar wind to the magnetosphere and ionosphere during a northward IMF. However, their formation mechanisms remain poorly understood and controversial. We report a mechanism identified from multiple-instrument observations of unusually bright, multiple TPAs and simulations from a high-resolution three-dimensional (3D) global MagnetoHydroDynamics (MHD) model. The observations and simulations show an excellent agreement and reveal that these multiple TPAs are generated by precipitating energetic magnetospheric electrons within field-aligned current (FAC) sheets. These FAC sheets are generated by multiple-flow shear sheets in both the magnetospheric boundary produced by Kelvin–Helmholtz instability between supersonic solar wind flow and magnetosphere plasma, and the plasma sheet generated by the interactions between the enhanced earthward plasma flows from the distant tail (less than −100 RE) and the enhanced tailward flows from the near tail (about −20 RE). The study offers insight into the complex solar wind-magnetosphere-ionosphere coupling processes under a northward IMF condition, and it challenges existing paradigms of the dynamics of the Earth’s magnetosphere.

The Steady Global Corona and Solar Wind: A Three-dimensional MHD Simulation with Turbulence Transport and Heating

2018 ◽  
Vol 865 (1) ◽  
pp. 25 ◽  
Author(s):  
Arcadi V. Usmanov ◽  
William H. Matthaeus ◽  
Melvyn L. Goldstein ◽  
Rohit Chhiber
Keyword(s):  
Solar Wind ◽  
Three Dimensional ◽  
Mhd Simulation ◽  
Turbulence Transport
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