Physics – Plasma Physics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh42a..04f&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH42A-04
Physics
Plasma Physics
[7509] Solar Physics, Astrophysics, And Astronomy / Corona, [7836] Space Plasma Physics / Mhd Waves And Instabilities
Scientific paper
The ever-increasing number and quality of observations of the hot corona (e.g. from RHESSI and SDO) and heliosphere (e.g. with STEREO) are ideally suited to investigate the role of waves and instabilities into the dynamics of rarefied magnetised plasmas and key flux rope phenomena of our Sun-Earth system. Small-scale transients originating and being released from the base of the Heliospheric Current Sheet (HCS) or further out in the inner heliosphere have now been shown, in part due to new observations from STEREO, to give a layered structure appearance to the HCS and to correspond to flux-rope and magnetic-island type plasmoids in the associated Heliospheric Plasma Sheet. We have now come to a greater appreciation of the importance of looking at the slow solar wind around the HCS as a boundary layer, where aspects of differential rotation-driven and continuous release of plasmoids could constitute some of the main differences in the comparison with the magnetospheric plasma sheet. New observations in the corona relate to the formation of those plasmoids and highlight the relevance of waves and instabilities in energetic events, such as flares and coronal mass ejections. SDO/AIA is now giving us the first observations of the temporally and spatially resolved evolution of the magnetic Kelvin-Helmholtz instability, which is seen developing at the surface of fast coronal mass ejecta. The non-linear effects, multi-scale and microphysical interactions inherent to the flow-driven instabilities can play a major role not only in the transient kinematics by enhancing the drag in localised regions, but also in the plasma entry across discontinuities.
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