Speaker
Sergiy Shelyag
(Northumbria University)
Description
The most energetic part of the Sun, interior, due to its
plasma parameters is hidden
below the solar surface and invisible to the observer.
Nevertheless, the solar
interior generates the energy and provokes atmospheric
magnetic activity. Despite
great progress in both observational and simulation methods,
the mechanism of energy
transport from the solar convection zone into the upper
atmosphere, and the
upper-atmospheric heating mechanism remain the main
unresolved problems in solar
physics. Waves in magnetic field concentrations were shown
to carry sufficient energy
to provide the chromospheric heating. They create currents,
which can be effectively
dissipated due to ion-neutral interaction in partially
ionised chromospheric plasma.
In this presentation, we analyse the role of non-ideal
plasma effects in the solar
atmospheric energy transport. Using numerical
magneto-hydrodynamic modelling we
create detailed models of magnetic flux tubes, which take
into account the effects of
partial ionisation and ion-neutral interaction in the solar
atmospheric plasma. We
show that compressible and incompressible oscillations in
solar magnetic fields are,
indeed, able to dissipate efficiently and provide sufficient
energy to compensate the
chromospheric radiative losses.
Primary author
Sergiy Shelyag
(Northumbria University)
