Speaker
Description
Solar eruptions are ubiquitous in the sun and play a significant role in space weather. With the advent of multi-view observations, we can gain a better understanding of the three-dimensional structure of these eruptive events and identify the various energetic processes involved. To fully grasp the physics behind these phenomena, it is essential to develop innovative simulations that complement these observations.
To this end, we have developed a numerical framework to model the evolution of active regions (ARs) using non-force-free magnetic field extrapolation, based on a magnetogram taken close to the onset of a flare, along with a stratified atmosphere. This presentation highlights the results of a solar eruption that occurred in NOAA AR 12241 on December 18, 2014.
Our simulation shows that a flux rope develops and rises self-consistently in the same direction as the observed eruption, without any arbitrary assumptions regarding the flux rope structure. With the aid of an algorithm that identifies and tracks the magnetic flux rope, we examine the dynamics of this structure and determine its kinematic properties. Additionally, we calculate synthetic extreme ultraviolet (EUV) emissions from different perspectives, allowing us to make direct comparisons with observations.
We also incorporate test particles into the model to identify particle acceleration sites and predict the location and shape of non-thermal emissions. Furthermore, we quantify the energy proportion that is transferred into heating, eruptions, and particle acceleration.
Our work not only deepens our understanding of the processes involved during a solar eruption but also clarifies energy distribution throughout the event. Ultimately, this represents a significant step forward in enhancing predictive capabilities for space weather, which is crucial for safeguarding technology and infrastructure on Earth.
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