Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aspc..424....3a&link_type=abstract
Proceedings of the 9th International Conference of the Hellenic Astronomical Society, proceedings of a conference held 20-24 Sep
Astronomy and Astrophysics
Astronomy
Scientific paper
One of the most important processes, responsible for many dynamical phenomena observed in the Sun, is the emergence of magnetic flux from the solar interior in active regions and the modification of the coronal magnetic field in response to the emergence. In fact, magnetic flux emergence might be responsible for the appearance of small-scale events (e.g., compact flares, plasmoids, active-region-associated X-ray brightenings) and large-scale events (e.g., X-class flares and CMEs). However, it is clear that the question of how exactly the magnetic fields rise through the convection zone of the Sun and emerge through the photosphere and chromosphere into the corona has still not been solved. Studying the process of flux emergence is an important step towards the understanding of the dynamic coupling between the solar interior and the outer solar atmosphere. This paper provides a brief review of some numerical models, which have been used to study the process of magnetic flux emergence into the outer solar atmosphere and the dynamics of associated explosive events.
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