Speaker
Mrs
Sofia-Paraskevi Moschou
(BISA-IASB & CmPA, KULeuven)
Description
Coronal rain phenomena are simulated in 3D setups in a magnetic configuration of a quadrupolar arcade system. A magnetohydrodynamic simulation is presented including three gain-loss terms, anisotropic thermal conduction, optically thin radiative losses, and parametrised heating to construct a realistic arcade configuration from chromospheric to coronal heights. Evaporated plasma from chromospheric and transition region heights eventually causes localised runaway condensation events. Plasma blobs are formed due to thermal instability, evolve dynamically in the heated arcade part and move gradually downwards due to gravitational instability. Unlike earlier 2.5D simulations, no formation of large scale prominence is observed here, but a continuous coronal rain develops which shows clear indications of Rayleigh-Taylor or interchange instability. The denser plasma located above the transition region falls down as the system seeks stability. Linear stability analysis is used in the non-linear regime to provide insight and to give a prediction of the system's evolution. After the plasma blobs descend through interchange, they move along the magnetic field lines in the lower coronal regions, where they are guided by the magnetic dips.
Primary author
Mrs
Sofia-Paraskevi Moschou
(BISA-IASB & CmPA, KULeuven)
