Modeling the Physical Connection Between the Solar Convection Zone and Corona

Details Modeling the Physical Connection Between the Solar Convection Zone and Corona Modeling the Physical Connection Between the Solar Convection Zone and Corona

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.0101a&link_type=abstract

American Astronomical Society, SPD meeting #42, #1.01; Bulletin of the American Astronomical Society, Vol. 43, 2011

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Scientific paper

How magnetic energy and flux emerges from below the surface into the solar atmosphere is a topic ripe for theoretical and observational investigation, particularly in the SDO era. Data from this mission is showing us that magnetic fields from the interior emerge through the surface, and energize the dynamic chromosphere and corona over a wide range of spatial and temporal scales. The interplay between granular-scale magnetic features, and large-scale structures from decaying active regions, for example, are seen to affect the large-scale solar magnetic field in complex ways. Being able to model these interactions in a way that captures the disparate spatial and temporal scales of the convection zone-to-corona system while simultaneously allowing for direct comparison with observations would be of enormous value in the effort to better understand the physics of coronal heating, the energetics of the solar wind, and the onset of magnetic eruptions (among other phenomena). In this lecture, I will summarize current progress in the effort to model the magnetic and energetic connection between the solar interior and atmosphere, and will describe the limitations and challenges inherent to this holistic approach.

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