The more we learn about the Sun, the more we can appreciate its essential complexity. Telescopes have taught us it is not an unblemished sphere. Multi-wavelength observations reveal its structured atmosphere, and ever-higher temporal and spatial resolutions expose its spectacular dynamics. Helioseismology penetrates its depths, and STEREO and Solar Orbiter views from off the Sun-Earth line yield the beginnings of a three-dimensional perspective. Underlying this complexity is solar magnetism - the consequence of a cycling dynamo and the cause of solar eruptions that originate in stressed and twisted magnetic fields. In this talk, I will highlight these two critical areas of solar physics, presenting recent advances and open questions associated with the solar dynamo and the storage and release of magnetic energy, and considering what might be learned from sustained observations from the Sun’s poles and from a truly global view on the magnetism of the solar corona.
Speaker: Sarah Gibson, National Corporation and University Corporation for Atmospheric Research
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Stanford, CA 94305
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