Fredagskollokvium: Magnetic flux emergence and reconnection in the solar atmosphere
Salvo Guglielmino, National Institute for Astrophysics (INAF) in Catania, Italy
Dr. Salvo Guglielmino, National Institute for Astrophysics (INAF), Italy.
The magnetic field is the main responsible for solar activity. Generated by a dynamo mechanism, it reaches the solar atmosphere and gives rise to a plethora of manifestations, including the appearance of sunspot and prominences. This process is known as magnetic flux emergence and involves all the atmospheric layers of the Sun in a variety of spatial scales, ranging from large active regions down to small magnetic flux concentrations, at the limit of the current instrumental capabilities.
At every scale, new magnetic flux emerges in a previously magnetized environment: this leads to the interaction between the emerging and pre-existing fields via magnetic reconnection. This physical process is able to convert magnetic energy into heat and kinetic energy of accelerated particles, giving rise to brighteness enhancements and plasma ejections in the solar atmosphere.
Here, I will discuss in particular small-scale flux emergence events and reconnection episodes, showing case studies where the response of the atmosphere due to new emerging flux released energies up to X-ray emission. I will emphasize the advantage of a synergetic approach between multi-wavelength observations to obtain a complete picture of the magnetic flux emergence from the photosphere to the corona.
Please join the seminar via Zoom at:
Meeting ID: 649 0476 2668