Multiwavelength studies of MHD waves in the solar chromosphere: An overview of recent results

The chromosphere is a thin layer of the solar atmosphere that bridges the relatively cool photosphere and the intensely heated transition region and corona. Compressible and incompressible waves propagating through the chromosphere can supply significant amounts of energy to the interface region and corona. In recent years an abundance of high-resolution observations from state-of-the-art facilities have provided new and exciting ways of disentangling the characteristics of oscillatory phenomena propagating through the dynamic chromosphere. Coupled with rapid advancements in magnetohydrodynamic wave theory, we are now in an ideal position to thoroughly investigate the role waves play in supplying energy to sustain chromospheric and coronal heating. Here, we review the recent progress made in characterising, categorising and interpreting oscillations manifesting in the solar chromosphere, with an impetus placed on their intrinsic energetics.Comment: 48 pages, 25 figures, accepted into Space Science Review

Experimental evidences and driving mechanisms for anisotropic misalignments in exchange coupled systems

Experimental evidence for misalignments between F anisotropy axes, AF anisotropy axes and the exchange bias field direction is shown in a CoFe/Ni 0.38 O0.62 system. The angular dependence of the remanent magnetization, the exchange bias field and the coercive field is studied as a function of the diluted NiO thickness. The exchange coupling leads to misalignments between the applied field during growth, the exchange bias field and the coercive field directions. It shows that two different interfacial spin frustrations are present, corresponding to pinned and unpinned spins contributions of the diluted NiO. Copyright EDP Sciences, SIF, Springer-Verlag Berlin Heidelberg 2011