Three-dimensional magnetohydrodynamic simulations on the interaction of interplanetary density pulses with the bow shock

2002 ◽  
Vol 9 (5) ◽  
pp. 1764-1774
Author(s):  
S. M. Park ◽  
D.-Y. Lee ◽  
K. W. Min ◽  
J. Seon
Keyword(s):  
Three Dimensional ◽  
Bow Shock ◽  
Magnetohydrodynamic Simulations

scholarly journals Three-dimensional simulations of solar magneto-convection including effects of partial ionization

2018 ◽  
Vol 618 ◽  
pp. A87 ◽  
Author(s):  
E. Khomenko ◽  
N. Vitas ◽  
M. Collados ◽  
A. de Vicente
Keyword(s):  
Magnetic Field ◽  
Three Dimensional ◽  
Ambipolar Diffusion ◽  
Solar Chromosphere ◽  
Degree Of Ionization ◽  
Poynting Flux ◽  
Complex Interactions ◽  
Low Degree ◽  
Magnetohydrodynamic Simulations ◽  
Three Dimensional Simulations

In recent decades, REALISTIC three-dimensional radiative-magnetohydrodynamic simulations have become the dominant theoretical tool for understanding the complex interactions between the plasma and magnetic field on the Sun. Most of such simulations are based on approximations of magnetohydrodynamics, without directly considering the consequences of the very low degree of ionization of the solar plasma in the photosphere and bottom chromosphere. The presence of a large amount of neutrals leads to a partial decoupling of the plasma and magnetic field. As a consequence, a series of non-ideal effects, i.e., the ambipolar diffusion, Hall effect, and battery effect, arise. The ambipolar effect is the dominant in the solar chromosphere. We report on the first three-dimensional realistic simulations of magneto-convection including ambipolar diffusion and battery effects. The simulations are carried out using the newly developed MANCHA3Dcode. Our results reveal that ambipolar diffusion causes measurable effects on the amplitudes of waves excited by convection in the simulations, on the absorption of Poynting flux and heating, and on the formation of chromospheric structures. We provide a low limit on the chromospheric temperature increase owing to the ambipolar effect using the simulations with battery-excited dynamo fields.

scholarly journals Filaments and striations: anisotropies in observed, supersonic, highly magnetized turbulent clouds

2019 ◽  
Vol 492 (1) ◽  
pp. 668-685 ◽  
Author(s):  
James R Beattie ◽  
Christoph Federrath
Keyword(s):  
Magnetic Field ◽  
Column Density ◽  
Three Dimensional ◽  
High Density ◽  
Systematic Analysis ◽  
Guide Field ◽  
Degree Of Anisotropy ◽  
Mach Numbers ◽  
Magnetohydrodynamic Simulations ◽  
The Magnetic Field

ABSTRACT Stars form in highly magnetized, supersonic turbulent molecular clouds. Many of the tools and models that we use to carry out star formation studies rely upon the assumption of cloud isotropy. However, structures like high-density filaments in the presence of magnetic fields and magnetosonic striations introduce anisotropies into the cloud. In this study, we use the two-dimensional power spectrum to perform a systematic analysis of the anisotropies in the column density for a range of Alfvén Mach numbers ($\operatorname{\mathcal {M}_{\text{A}}}=0.1{\!-\!10}$) and turbulent Mach numbers ($\operatorname{\mathcal {M}}=2{\!-\!20}$), with 20 high-resolution, three-dimensional turbulent magnetohydrodynamic simulations. We find that for cases with a strong magnetic guide field, corresponding to $\operatorname{\mathcal {M}_{\text{A}}}\lt 1$, and $\operatorname{\mathcal {M}}\lesssim 4$, the anisotropy in the column density is dominated by thin striations aligned with the magnetic field, while for $\operatorname{\mathcal {M}}\gtrsim 4$ the anisotropy is significantly changed by high-density filaments that form perpendicular to the magnetic guide field. Indeed, the strength of the magnetic field controls the degree of anisotropy and whether or not any anisotropy is present, but it is the turbulent motions controlled by $\operatorname{\mathcal {M}}$ that determine which kind of anisotropy dominates the morphology of a cloud.

scholarly journals Plasma environment of magnetized asteroids: a 3-D hybrid simulation study

2006 ◽  
Vol 24 (1) ◽  
pp. 407-414 ◽  
Author(s):  
S. Simon ◽  
T. Bagdonat ◽  
U. Motschmann ◽  
K.-H. Glassmeier
Keyword(s):  
Solar Wind ◽  
Three Dimensional ◽  
Hybrid Simulation ◽  
Interaction Region ◽  
Bow Shock ◽  
The Other ◽  
Simulation Code ◽  
Kinetic Effects ◽  
Intrinsic Magnetic Moment ◽  
The One

Abstract. The interaction of a magnetized asteroid with the solar wind is studied by using a three-dimensional hybrid simulation code (fluid electrons, kinetic ions). When the obstacle's intrinsic magnetic moment is sufficiently strong, the interaction region develops signs of magnetospheric structures. On the one hand, an area from which the solar wind is excluded forms downstream of the obstacle. On the other hand, the interaction region is surrounded by a boundary layer which indicates the presence of a bow shock. By analyzing the trajectories of individual ions, it is demonstrated that kinetic effects have global consequences for the structure of the interaction region.

scholarly journals Three-Dimensional MHD Simulations of a Subcluster Plasma Moving in Turbulent ICM

2006 ◽  
Vol 2 (S235) ◽  
pp. 189-189
Author(s):  
N. Asai ◽  
N. Fukuda ◽  
R. Matsumoto
Keyword(s):  
Heat Conduction ◽  
Magnetic Fields ◽  
Three Dimensional ◽  
Cold Fronts ◽  
Mhd Simulations ◽  
Anisotropic Heat Conduction ◽  
Magnetohydrodynamic Simulations

AbstractWe carried out 3D magnetohydrodynamic simulations of a subcluster moving in turbulent ICM by including anisotropic heat conduction. Since magnetic fields stretched along the subcluster surface suppress the heat conduction across the front, cold fronts are formed and sustained.

scholarly journals The magneto-Rayleigh–Taylor instability in dynamic z pinches

2001 ◽  
Vol 19 (4) ◽  
pp. 527-540 ◽  
Author(s):  
M.R. DOUGLAS ◽  
J.S. DE GROOT ◽  
R.B. SPIELMAN
Keyword(s):  
Peak Plasma ◽  
Dominant Role ◽  
Three Dimensional ◽  
Vacuum Field ◽  
Nonlinear Growth ◽  
Spatial Uniformity ◽  
Rayleigh Taylor Instability ◽  
Magnetohydrodynamic Simulations ◽  
Insight Into ◽  
Initial Seeding

The magneto-Rayleigh–Taylor (MRT) instability limits the performance of dynamic z pinches. This instability develops at the plasma-vacuum/field interface, growing in amplitude throughout the implosion, thereby reducing the peak plasma velocity and spatial uniformity at stagnation. MRT instabilities are believed to play a dominant role in the case of high wire number arrays, gas puffs and foils. In this article, the MRT instability is discussed in terms of initial seeding, linear and nonlinear growth, experimental evidence, radiation magnetohydrodynamic simulations, and mitigating schemes. A number of experimental results are presented, where the mitigating schemes have been realized. In general, the problem is inherently three dimensional, but two-dimensional simulations together with theory and experiment enhance our physical understanding and provide insight into future load design.

scholarly journals Three‐dimensional Magnetohydrodynamic Simulations of Spherical Accretion

2002 ◽  
Vol 566 (1) ◽  
pp. 137-147 ◽  
Author(s):  
Igor V. Igumenshchev ◽  
Ramesh Narayan
Keyword(s):  
Three Dimensional ◽  
Magnetohydrodynamic Simulations
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