Context. Oscillations in coronal loops are usually interpreted in terms of uncoupled magnetohydrodynamic (MHD) waves. Examples of these waves are standing transverse motions, interpreted as the kink MHD modes, and propagating slow modes, commonly reported at the loop footpoints. Aims. Here we study a simple system in which fast and slow MHD waves are coupled. The goal is to understand the finge...

In this paper we perform an analysis of the wave structure of the ideal magnetohydrodynamic (MHD) equations. We present an analytical expression of the nonlinearity term associated to each characteristic field derived from a scaled version of the complete system of eigenvectors proposed by Brio andWu [M. Brio, C.C. Wu, An upwind differencing scheme for the equations of ideal magnetohydrodynamic...

Abstract We present a study of density fluctuations in coronal holes. used reduced magnetohydrodynamic (RMHD) model that incorporated observationally constrained to determine whether holes can enhance Alfvén wave reflection and dissipation, thereby heating driving the fast solar wind. show results for two models background atmosphere. Each is solution momentum equation includes effects pressure...

Abstract The evolution of the Kelvin–Helmholtz instability (KHI) and magnetohydrodynamic (MHD) wave emission is investigated at shear-flow boundaries magnetized plasmas. While MHD has been suggested to be only possible during nonlinear stages, we find that there also significant KHI’s linear stages. These emitted waves may have stronger impacts than KHI surface since they can act transport ener...

The equations of the three-dimensional viscous, compressible, and heat conducting magnetohydrodynamic flows are considered in a bounded domain. The viscosity coefficients and heat conductivity can depend on the temperature. A solution to the initial-boundary value problem is constructed through an approximation scheme and a weak convergence method. The existence of a global variational weak sol...

Abstract In this paper, we provide clear direct evidence of multiple concurrent higher-order magnetohydrodynamic (MHD) modes in circular and elliptical sunspots by applying both proper orthogonal decomposition (POD) dynamic mode (DMD) techniques on solar observational data. These are well documented validated the areas fluid mechanics, hydraulics, granular flows but relatively new to field phys...

Linear and nonlinear gyrokinetic simulations with the GENE code F. Jenko et al., Phys. Plasmas 7, 1904 2000 for tokamak edge plasmas as well as for stellarator core plasmas are presented, shedding light on the behavior of plasma microturbulence under near-separatrix or nonaxisymmetric conditions. To this aim, the required geometric coefficients are inferred directly from the magnetohydrodynamic...

The linearized relativistic magnetohydrodynamic (RMHD) equations describing a uniform axially magnetized cylindrical relativistic jet spine embedded in a uniform axially magnetized relativistically moving sheath are derived. The displacement current is retained in the equations so that effects associated with Alfvén wave propagation near light speed can be studied. A dispersion relation for the...

We present ECOM (Equilibrium solver via COnformal Mapping), a fast and accurate fixed boundary solver for toroidally axisymmetric magnetohydrodynamic equilibria with or without a toroidal flow. ECOM combines conformal mapping and Fourier and integral equation methods on the unit disk to achieve exponential convergence for the poloidal flux function aswell as its first and second partial derivat...

Hypermassive neutron stars (HMNSs)--equilibrium configurations supported against collapse by rapid differential rotation--are possible transient remnants of binary neutron-star mergers. Using newly developed codes for magnetohydrodynamic simulations in dynamical spacetimes, we are able to track the evolution of a magnetized HMNS in full general relativity for the first time. We find that secula...