Coronal seismology, a new field of solar physics that emerged over the last 5 years, provides unique information on basic physical properties of the solar corona. The inhomogeneous coronal plasma supports a variety of magnetohydrodynamics (MHD) wave modes, which manifest themselves as standing waves (MHD oscillations) and propagating waves. Here, we briefly review the physical properties of obs...

Turbulence in an incompressible fluid with and without a magnetic field as well as moderately compressible MHD turbulence are compared. The results of three numerical simulation models in three dimensions of resolution up to 512 are used for this purpose. The compatibility of the spectra of all three models with the Kolmogorov spectrum is confirmed. For the magnetohydrodynamic (MHD) models the ...

BACKGROUND Studies that examined dietary energy requirements (DERs) of patients undergoing maintenance hemodialysis (MHD) have shown mixed results. Many studies reported normal DERs, but some described increased energy needs. DERs in MHD patients have been estimated primarily from indirect calorimetry and from nitrogen balance studies. The present study measured DERs in MHD patients on the basi...

We present the critical conditions for hot trans-fast magnetohydrodynamical (MHD) flows in a stationary and axisymmetric black-hole magnetosphere. To accrete onto the black hole, the MHD flow injected from a plasma source with low velocity must pass through the fast magnetosonic point after passing through the “inner” or “outer” Alfvén point. We find that a trans-fast MHD accretion solution rel...

The beta limit by the ideal MHD instabilities (so-called “MHD stability beta limit”) for helical plasmas is studied by a hierarchy integrated simulation code. A numerical model for the effect of the MHD instabilities is introduced such that the pressure profile is flattened around the rational surface due to the MHD instabilities. The width of the flattening of the pressure gradient is determin...

Effects of a toroidal rotation are investigated numerically on the stability of the MHD modes in the edge pedestal, which relate to the type-I edge-localized mode (ELM). A new linear MHD stability code MINERVA is developed for solving the Frieman-Rotenberg equation, which is the linear ideal MHD equation with flow. As the result of the stability analysis, it is revealed that the sheared toroida...

The authors tested the thesis that people find the Monty Hall dilemma (MHD) hard because they fail to understand the implications of its causal structure, a collider structure in which 2 independent causal factors influence a single outcome. In 4 experiments, participants performed better in versions of the MHD involving competition, which emphasizes causality. This manipulation resulted in mor...

Magnetohydrodynamic (MHD) turbulence is pervasive in astrophysical systems. Recent highresolution numerical simulations suggest that the energy spectrum of strong incompressible MHD turbulence is E(k⊥) ∝ k ⊥ . So far, there has been no phenomenological theory that simultaneously explains this spectrum and satisfies the exact analytic relations for MHD turbulence due to Politano & Pouquet. Indee...

The magnetohydrodynamic (MHD) is the study of the interaction of electrically conducting fluids and electromagnetic fields. This paper presents the numerical modelling of the coupling electromagnetichydrodynamic phenomena using the Finite volume Method (FVM) in cylindrical coordinate and the stream vorticity formulation ξ, ψ in two-dimensional in an annular induction MHD pump. The magnetic indu...

We describe a formulation of two-dimensional geometrical shock dynamics (GSD) suitable for ideal magnetohydrodynamic (MHD) fast shocks under magnetic fields of general strength and orientation. The resulting area–Mach-number–shock-angle relation is then incorporated into a numerical method using pseudospectral differentiation. The MHD-GSD model is verified by comparison with results from nonlin...