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...

We study the fundamental physics of cascades and spectra in two-dimensional (2D) Cahn-Hilliard-Navier-Stokes (CHNS) turbulence, and compare and contrast this system with 2D magnetohydrodynamic (MHD) turbulence. The important similarities include basic equations, ideal quadratic invariants, cascades, and the role of linear elastic waves. Surface tension induces elasticity, and the balance betwee...

Perhaps the most intriguing result of Planck’s dust-polarization measurements is the observation that the power in the E-mode polarization is twice that in the B mode, as opposed to pre-Planck expectations of roughly equal dust powers in E and B modes. Here we show how the Eand Bmode powers depend on the detailed properties of the fluctuations in the magnetized interstellar medium. These fluctu...

In this paper we study the temporal evolution of linear MHD waves excited by footpoint motions using an ideal, pressureless slab model for coronal loops. We choose the footpoint motions to be polarised normal to the magnetic flux surfaces such that only fast waves are driven directly, including the so-called quasi-modes. We have derived a formal analytical solution as a superposition of eigenmo...

In this article, we present an entrainment-based model for predicting the flow and power output of finite-length wind farms. The is extension three-layer approach Luzzatto-Fegiz & Caulfield ( Phys. Rev. Fluids , vol. 3, 2018, 093802) farms infinite length, assumes dependence key quantities, such as farm bulk velocity, on streamwise distance from entrance. To assist our analysis validate pro...

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 ...

The Taylor microscale is a fundamental length scale in turbulent fluids, representing the end of fluid properties and onset dissipative processes. can also be used to evaluate Reynolds number classical turbulence theory. Although solar wind weakly collisional, it approximately behaves as magnetohydrodynamic (MHD) at scales larger than kinetic scale. As result, theory formalisms are often study ...

The Study of river water quality interation with lakes and dam reservoirs is important from anexploitation point of view. When river water with different densities enters a lake or dam reservoir,underflow density current phenomenon occurs. Because of the density, so understandingdifferent arrays of this phenomenon Seems necessary for checking erosion and sedimentationprocesses and their managem...

Spectral properties of a fully compressible solar wind Hall Magnetohydrodynamic plasma are investigated by means of time dependent three dimensional Hall MHD simulations. Our simulations, in agreement with spacecraft data, identify a spectral break in turbulence spectra at characteristic length-scales associated with electromagnetic fluctuations that are smaller than the ion gyroradius. In this...

Magnetic reconnection is of great interest in many space and laboratory plasmas [1,2], and has been studied extensively for more than four decades. The most important question is that of the reconnection rate. The process of magnetic reconnection, is so complex, however, that this question is still not completely resolved, even within the simplest possible canonical model: twodimensional (2D) i...