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The Sun's Dynamic Extended Corona Observed in Extreme Ultraviolet View all abstracts by submitter

Dan Seaton   Submitted: 2021-05-20 16:58

The "middle corona" is a critical transition between the highly disparate physical regimes of the lower and outer solar corona. Nonetheless, it remains poorly understood due to the difficulty of observing this faint region (1.5-3 solar radii). New observations from the GOES Solar Ultraviolet Imager in August and September 2018 provide the first comprehensive look at this region's characteristics and long-term evolution in extreme ultraviolet (EUV). Our analysis shows that the dominant emission mechanism here is resonant scattering rather than collisional excitation, consistent with recent model predictions. Our observations highlight that solar wind structures in the heliosphere originate from complex dynamics manifesting in the middle corona that do not occur at lower heights. These data emphasize that low-coronal phenomena can be strongly influenced by inflows from above, not only by photospheric motion, a factor largely overlooked in current models of coronal evolution. This study reveals the full kinematic profile of the initiation of several coronal mass ejections, filling a crucial observational gap that has hindered understanding of the origins of solar eruptions. These new data uniquely demonstrate how EUV observations of the middle corona provide strong new constraints on models seeking to unify the corona and heliosphere.

Authors: Daniel B. Seaton, J. Marcus Hughes, Sivakumara K. Tadikonda, Amir Caspi, Craig DeForest, Alexander Krimchansky, Neal E. Hurlburt, Ralph Seguin, Gregory Slater
Projects: GOES/SUVI,SoHO-LASCO

Publication Status: Accepted for publication in Nature Astronomy
Last Modified: 2021-05-23 10:47
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