Vyacheslav Lukin (National Science Foundation)

The magnetism of the solar surface

Az előadás kivonata: The highly dynamic and constantly evolving surface of our nearest star, the Sun, is threaded by magnetic fields that emerge, self-organize into large-scale structures, and occasionally erupt producing solar flares and coronal mass ejections.  These magnetic fields permeate the plasma of the solar atmosphere that varies from cold, dense, weakly ionized plasma of the chromosphere just above the solar surface to the hot and tenuous plasma of the solar corona.  Throughout, magnetic field structures embedded in the plasma undergo cycles of energy accumulation driven by convective motions below, inevitably followed by magnetic energy release into plasma flows, heating, radiation, and high energy particle acceleration.  A process that often underlies both the large-scale magnetic structure formation and the magnetic energy release is magnetic reconnection, the process associated with changes in magnetic topology within the electrically conducting plasma medium.  We discuss the known and the unknown in magnetic reconnection research in the solar atmosphere and other contexts, and zoom into properties of magnetic substructures undergoing magnetic reconnection in partially ionized plasmas of the lower solar atmosphere.

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