A direct numerical simulation of decaying, homogeneous and isotropic turbulence of the incompressible Hall magnetohydrodynamic equations is carried out to clarify its statistical natures. Contributions of small scales to the statistics are examined. It is shown that the probability density function (PDF) of the enstrophy density is well characterized by the Gaussian distribution when the short ...

Magnetohydrodynamic (MHD) turbulence in the solar wind is observed to show the spectral behavior of classical Kolmogorov fluid turbulence over an inertial subrange and departures from this at short wavelengths, where energy should be dissipated. Here we present the first measurements of the electric field fluctuation spectrum over the inertial and dissipative wavenumber ranges in a β & 1 plasma...

Using data obtained by the high temporal and spatial resolution Rapid Oscillations in the Solar Atmosphere instrument on the Dunn Solar Telescope, we investigate at an unprecedented level of detail transverse oscillations in chromospheric fine structures near the solar disk center. The oscillations are interpreted in terms of propagating and standing magnetohydrodynamic kink waves. Wave charact...

We have drawn together in this paper a collection of magnetohydrodynamic (MHD) problems that will provide researchers who have interests in modeling MHD phenomena with a battery of tests (a \test suite") for calibrating their numerical algorithms. Use of these tests will provide a common reference for comparison of di erent numerical MHD algorithms. The test suite includes both one and two dime...

The heating of the solar corona has been a fundamental astrophysical issue for over sixty years. Over the last decade in particular, space-based solar observatories (Yohkoh, SOHOandTRACE) have revealed the complex and often subtlemagnetic-field and plasma interactions throughout the solar atmosphere in unprecedented detail. It is now established that any energy release mechanism is magnetic in ...

We propose a mechanism to make gravitational waves (GWs) visible in the electromagnetic domain. Gravitational waves that propagate through a strongly magnetized plasma interact with the plasma through its anisotropic stress-energy tensor and excite magnetohydrodynamic (MHD) wave modes. In catastrophic events such as the merger of a double neutron star binary, a large fraction of the total bindi...

We derive the closed system of averaged magnetohydrodynamic (MHD) equations for general oscillating flows. The used small parameter of our asymptotic theory is the dimensionless inverse frequency, and the leading term for a velocity field is chosen to be purely oscillating. The employed mathematical approach combines the twotiming method and the notion of a distinguished limit. The properties o...

We propose a phenomenological model for incompressible magnetohydrodynamic turbulence. We argue that nonlinear-wave interaction weakens as the energy cascade proceeds to small scales, however, the anisotropy of fluctuations along the large-scale magnetic field increases, which makes turbulence strong at all scales. To explain the weakening of the interaction, we propose that smallscale fluctuat...

Transport is studied for the kinetically stabilized tandem mirror, an attractive magnetic confinement device for achieving a steady-state burning plasma. For a magnetohydrodynamic stable system, three different radial transport models with Bohm, gyro-Bohm, and electron temperature gradient ETG scaling are derived. As a conservative estimate, numerical coefficients in the models are taken to be ...