Determining the chromospheric magnetic field vector on the Sun strategic analysis using comprehensive simulations

Important results from the project

Studying the physical processes that take place in our star is important. Our society is directly affected through phenomena like solar energetic particles, geomagnetically induced currents and ionospheric disturbances. These phenomena are caused by the solar activity. By studying fundamental processes that drive solar activity help us predict these events but also understand better not only our star, but other types of stars as well. This project focuses on realistic modelling of the solar atmosphere and accurate retrieval of information from the solar spectra.

Expected long term effects

Retrieving the information from the solar spectra requires intricate theoretical modelling. It starts with three dimensional realistic magnetohydrodynamic modeling of the atmosphere. Thanks to this grant we made a great step forward to creating more complete models that can be used for studying different features visible on the Sun. An example of our results is the synthetic jet visible in figure under this link (https://dubshen.astro.su.se/~sdani/agu/600000h_55_cam1r.jpeg). It is named peacock jet because it spreads as a peacocks tail.

Approach and implementation

The second step in studying solar atmosphere is using these three-dimensional models to generate synthetic images and spectra that are directly compared with solar observations. Finally, properties of the material and magnetic field in the solar atmosphere cannot be measured directly. They are instead determined from observed spectra through a process called inversion. In this project, we combined inversions with machine learning to get better and faster results.