We have argued that magnetohydrodynamic (MHD) turbulence in an accretion disk naturally produces hoop-stresses, and that in a geometrically-thick flow these stresses could both drive and collimate an outflow. We based this argument on an analogy of turbulent MHD fluids to viscoelastic fluids, in which azimuthal shear flow creates hoop-stresses that cause a variety of flow phenomena, including t...

We have argued that MHD turbulence in an accretion disk naturally produces hoop-stresses, and that in a geometrically-thick flow these stresses could both drive and collimate an outflow. We based this argument on an analogy of turbulent MHD fluids to viscoelastic fluids, in which azimuthal shear flow creates hoop-stresses that cause a variety of flow phenomena, including the Weissenberg effect ...

Backgrounds: Patients with maintenance hemodialysis (MHD) have a high risk of cardiovascular disease, which is the leading cause of morbidity and mortality. The aim of the present study was to explore the relationship between the sodium gradient and the water load of MHD patients. Methods: Eighty one MHD patients were selected in the study. The serum sodium concentration, sodium gradient, inter...

In this paper, we develop a lattice Boltzmann model for relativistic magnetohydrodynamics (MHD). Even though the model is derived for resistive MHD, it is shown that it is numerically robust even in the high conductivity (ideal MHD) limit. In order to validate the numerical method, test simulations are carried out for both ideal and resistive limits, namely the propagation of Alfvén waves in th...

We report on experimental observations that the two-fluid Hall dynamo plays an important role in plasma relaxation. Measurements of the Hall effect during relaxation are made in the plasma core and edge. The Hall dynamo is found to be small at the edge ( ! r /a " 0.85) but increases substantially towards the interior (r/a=0.82) as measured by probes. In the high-temperature plasma core (r/a=0.3...

The solar photosphere is a partially ionized medium with collisions between electrons, various metallic ions and neutral hydrogen playing an important role in the momentum and energy transport in the medium. Furthermore, the number of neutral hydrogen atom could be as large as 10 times the number of plasma particles in the lower photosphere. The non-ideal MHD effects, namely Ohm, Ambipolar and ...

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...

Cosmic rays scatter off magnetic irregularities (Alfvén waves) with which they are resonant, that is waves of wavelength comparable to their gyroradii. These waves may be generated either by the cosmic rays themselves, if they stream faster than the Alfvén speed, or by sources of MHD turbulence. Waves excited by streaming cosmic rays are ideally shaped for scattering, whereas the scattering eff...

Achromatic breaks in afterglow light curves of gamma-ray bursts (GRBs) arise naturally when the product of the jet’s Lorentz factor γ and opening angle Θ j satisfies γΘ j ≫ 1. Magnetohydrodynamic (MHD) simulations of collimated GRB jets generally give γΘ j . 1, suggesting that MHD models are incapable of explaining jet breaks. We work within the collapsar paradigm and use axisymmetric relativis...