Speaker
Pia Zacharias
(University of Oslo)
Description
Observations of solar transition region emission lines reveal the presence of
redshifts up to temperatures of about 300,000 K and blueshifts for higher
temperatures. The apparent large downward flows in the lower transition region would
lead to an emptying of the corona, in contrast to what is being observed, thus some
mechanism must be responsible for maintaining the mass balance between the
photosphere and corona. We use the Bifrost stellar atmosphere code to perform 3D
radiation MHD simulations of the solar atmosphere and to study the temporal evolution
of mass flows into and out of the solar corona. By adding tracer particles to the
simulations and analyzing their characteristics over time, we provide new insights on
the physical processes driving these mass flows and on their role in the
chromosphere-corona mass cycle.
Primary author
Pia Zacharias
(University of Oslo)
