Conveners
Poster Session 7.3
- Georgia Tsiropoula (National Observatory of Athens)
The propagation of Alfven waves with periods > 10 s in the stratified isothermal atmosphere has been considered. Based on the numerical simulation the dependence of the wave energy flux on the height at different values of wave periods has been calculated. It has been shown that the so-called tuning points («cutoff frequencies») could not be used for the description of wave energy flux. The...
The equilibrium of the axisymmetric cylindrical magnetic flux rope under solar coronal conditions in the light of the paradigms of Severny and Parker connected with the existence of neutralized and non-neutralized electric currents in the solar photosphere is considered. Based on the generalized Gold-Hoyle force-free magnetic field configuration it has been shown that only the non-shielded...
Using data from the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory (HMI/SDO) on the magnetic field vector in the solar photosphere, we analyzed the structure of magnetic fields and vertical electric currents in six active regions (ARs) with different levels of flare activity. Decomposition of the transverse magnetic field vector into two components allowed us to...
Coronal loops are building blocks of solar active regions. However, their formation mechanism is still not well understood. Here we present direct observational evidence for the formation of coronal loops through magnetic reconnection as new magnetic fluxes emerge into the solar atmosphere. Extreme-ultraviolet observations of the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics...
Structures and heating mechanism of microflares have been unclear, but which is promising to be resolved with coming Solar Orbiter data combined with other ground-based telescopes of ultrahigh temporal and spatial resolution observations. Here, we analyze 3D magnetic structures and heating mechanism of a microflare based on three-dimensional radiative magnetohydrodynamic simulation of a solar...
The triggering process for prominence instability and consequent CMEs is not fully understood. Prominences are maintained by the Lorentz force against the gravity, therefore reduction of the prominence mass due to the coronal rain may cause the change of the force balance and hence destabilization of the structures.
We aim to study the observational evidence of the influence of coronal rain...
High-resolution solar observations show the complex structure of the magnetohydrodynamic (MHD) wave motion. We apply the Proper Orthogonal Decomposition (POD) and Dynamic Mode Decomposition (DMD) techniques to identify the dominant MHD wave modes in a sunspot with a circular cross-sectional shape, using the intensity time series. The POD technique was used to find modes that are spatially...
