Maria Valeria Sieyra
Characterising solar eruptions through data-constrained MHD simulations
Solar eruptions are ubiquitous in the sun and are one of the leading actors of space weather. Motivated by what drives eruptive processes and to better understand the coupling between active region magnetic topology and thermodynamical variables, we develop a numerical framework for modelling ARs evolution. We consider different extrapolation techniques based on an HMI magnetogram. Here, I will present the results of an eruption that occurred in NOAA AR 12241 on December 18, 2014 using a non force free extrapolation. We find that a flux rope self-consistently develops and rises. With the aid of an algorithm that identifies and tracks this structure, we study the dynamics of the magnetic flux rope and determine the kinematical properties. We also reproduce synthetic EUV emissions from different points of view that can be directly compared with observations. With the aim of identifying particle acceleration sites and to predict the location and shape of non-thermal emission, we also add test particles to the model. This work takes us a step closer to understanding the processes involved during the eruption.
Event Timeslots (1)
Friday
-
PDF
Characterising solar eruptions through data-constrained MHD simulations
