We study decaying magnetohydrodynamics (MHD) turbulence stemming from the evolution of the Taylor-Green flow generalized recently to MHD, with equal viscosity and magnetic resistivity and up to equivalent grid resolutions ...

For a molecular cloud clump to form stars some transport of magnetic flux is required from the denser, inner regions to the outer regions of the cloud, otherwise this can prevent the collapse. Fast magnetic reconnection ...

We have developed a new three-dimensional magnetohydrodynamic (MHD) solar wind model coupled to the Space Weather Modeling Framework (SWMF), that solves for the different electron and proton temperatures. The collisions ...

The ambient of the cloud that gives rise to the process of star formationconsisted of: turbulence, magnetic field and dust. In general, in the process of star formation there is the formation of an accretion disk whose ...

In stably stratified stars, numerical magnetohydrodynamics simulations have shown that arbitrary initial magnetic fields evolve into stable equilibrium configurations, usually containing nearly axisymmetric, linked ...

Se quiere investigar las inestabilidades paramétricas de una onda de Alfv¶en circularmente polarizada que se propaga en un plasma de electrones protones y partículas alfa a lo largo de un campo magnético de fondo. El interés ...

We present an extensive analysis of the 850 μm polarization maps of the SCUBA Polarimeter Legacy (SCUPOL) Catalogue produced by Matthews et al., focusing exclusively on the molecular clouds and star-forming regions. For ...

During the final three of the five consecutive and similar Cassini Titan flybys T55–T59 we observe a region characterized by high plasma densities (electron densities of 1–8 cm3 ) in the tail/nightside of Titan. This region ...

The combination of Differential Emission Measure Tomography (DEMT) with extrapolation of the photospheric magnetic field allows determinatio/n of the electron density and electron temperature along individual magnetic field ...