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Solar Physics

Dr. Gregory Fleishman.

The key driver of all the aspects of solar activity is the magnetic field. The solar magnetism group at KIS studies the magnetic field topology and the evolution throughout the only visible part of the Sun: the atmosphere. From the photosphere, through the chromosphere and all the way up in the corona, the members of our group rely on spectropolarimetric inversions, radio observations, MHD simulations, and magnetic field extrapolations to infer, reconstruct and, most importantly, understand the magnetic field of our host star. 

The focus of our research are the active regions: places where the strong magnetic fields protrude through the solar photosphere. We follow the evolution of these active regions using photospheric and chromospheric observations and numerical simulations (R. Schlichenmaier), reconstruct their 3D structure using radio observations and magnetic field extrapolations (G. Fleishman), and attempt to precisely measure their magnetic fields and electric currents (J.M. Borrero). Our researchers are also studying the magnetic field in the so-called quiet Sun regions, using Zeeman (J.M. Borrero) and Hanle (I. Milic) effects. To develop and employ state-of-the-art observation and analysis techniques, the group for solar magnetism actively collaborates with other KIS groups and departments. 

 


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