Model of the solar wind interaction with the local interstellar medium: Numerical solution of self-consistent problem

1993 ◽  
Vol 98 (A9) ◽  
pp. 15157 ◽  
Author(s):  
V. B. Baranov ◽  
Yu. G. Malama
Keyword(s):  
Solar Wind ◽  
Interstellar Medium ◽  
Numerical Solution ◽  
Local Interstellar Medium ◽  
Solar Wind Interaction ◽  
Self Consistent ◽  
Consistent Problem

scholarly journals Pickup Ion Effect of the Solar Wind Interaction with the Local Interstellar Medium

2016 ◽  
Vol 767 ◽  
pp. 012020 ◽  
Author(s):  
N. V. Pogorelov ◽  
M. C. Bedford ◽  
I. A. Kryukov ◽  
G. P. Zank
Keyword(s):  
Solar Wind ◽  
Interstellar Medium ◽  
Local Interstellar Medium ◽  
Solar Wind Interaction

Unsteady processes in the solar wind interaction with the local interstellar medium

2007 ◽  
Author(s):  
N. V. Pogorelov ◽  
S. N. Borovikov ◽  
I. A. Kryukov ◽  
D. Shaikh ◽  
G. P. Zank
Keyword(s):  
Solar Wind ◽  
Interstellar Medium ◽  
Local Interstellar Medium ◽  
Solar Wind Interaction ◽  
Unsteady Processes

scholarly journals Modelling the solar wind interaction with Mercury by a quasi-neutral hybrid model

2003 ◽  
Vol 21 (11) ◽  
pp. 2133-2145 ◽  
Author(s):  
E. Kallio ◽  
P. Janhunen
Keyword(s):  
Solar Wind ◽  
Plasma Physics ◽  
Hybrid Model ◽  
Space Plasma ◽  
Physical Processes ◽  
Space Plasma Physics ◽  
Solar Wind Interaction ◽  
Plasma Parameters ◽  
Advantages And Disadvantages ◽  
Self Consistent

Abstract. Quasi-neutral hybrid model is a self-consistent modelling approach that includes positively charged particles and an electron fluid. The approach has received an increasing interest in space plasma physics research because it makes it possible to study several plasma physical processes that are difficult or impossible to model by self-consistent fluid models, such as the effects associated with the ions’ finite gyroradius, the velocity difference between different ion species, or the non-Maxwellian velocity distribution function. By now quasi-neutral hybrid models have been used to study the solar wind interaction with the non-magnetised Solar System bodies of Mars, Venus, Titan and comets. Localized, two-dimensional hybrid model runs have also been made to study terrestrial dayside magnetosheath. However, the Hermean plasma environment has not yet been analysed by a global quasi-neutral hybrid model. In this paper we present a new quasi-neutral hybrid model developed to study various processes associated with the Mercury-solar wind interaction. Emphasis is placed on addressing advantages and disadvantages of the approach to study different plasma physical processes near the planet. The basic assumptions of the approach and the algorithms used in the new model are thoroughly presented. Finally, some of the first three-dimensional hybrid model runs made for Mercury are presented. The resulting macroscopic plasma parameters and the morphology of the magnetic field demonstrate the applicability of the new approach to study the Mercury-solar wind interaction globally. In addition, the real advantage of the kinetic hybrid model approach is to study the property of individual ions, and the study clearly demonstrates the large potential of the approach to address these more detailed issues by a quasi-neutral hybrid model in the future.Key words. Magnetospheric physics (planetary magnetospheres; solar wind-magnetosphere interactions) – Space plasma physics (numerical simulation studies)

scholarly journals Three-dimensional simulations of turbulent spectra in the local interstellar medium

2007 ◽  
Vol 14 (4) ◽  
pp. 351-359 ◽  
Author(s):  
D. Shaikh ◽  
G. P. Zank
Keyword(s):  
Interstellar Medium ◽  
Three Dimensional ◽  
Density Fluctuations ◽  
Spectral Energy ◽  
Local Interstellar Medium ◽  
Laboratory Plasmas ◽  
Self Consistent ◽  
Supersonic Plasma ◽  
Turbulent Spectra ◽  
Three Dimensional Simulations

Abstract. Three-dimensional time dependent numerical simulations of compressible magnetohydrodynamic fluids describing super-Alfvénic, supersonic and strongly magnetized space and laboratory plasmas show a nonlinear relaxation towards a state of near incompressibility. The latter is characterized essentially by a subsonic turbulent Mach number. This transition is mediated dynamically by disparate spectral energy dissipation rates in compressible magnetosonic and shear Alfvénic modes. Nonlinear cascades lead to super-Alfvénic turbulent motions decaying to a sub-Alfvénic regime that couples weakly with (magneto)acoustic cascades. Consequently, the supersonic plasma motion is transformed into highly subsonic motion and density fluctuations experience a passive convection. This model provides a self-consistent explaination of the ubiquitous nature of incompressible magnetoplasma fluctuations in the solar wind and the interstellar medium.

Interaction of the solar wind with the local interstellar medium: A multifluid approach

1996 ◽  
Vol 101 (A10) ◽  
pp. 21639-21655 ◽  
Author(s):  
G. P. Zank ◽  
H. L. Pauls ◽  
L. L. Williams ◽  
D. T. Hall
Keyword(s):  
Solar Wind ◽  
Interstellar Medium ◽  
Local Interstellar Medium
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