Authors: A.A. van Ballegooijen
Affiliation: Harvard-Smithsonian Center for Astrophysics
One of the primary objectives of the LWS program is to understand how energy
is injected into the corona, how it is stored there, and how it is released.
This requires determining the geometry of the coronal magnetic field and its
evolution subject to external forcing and energy dissipation. I will discuss
how magnetic-field measurements from SDO/HMI and coronal images from SDO/AIA
will be used to advance our understanding of 3D coronal magnetic structure and
evolution. I will focus on non-potential structures associated with filaments
and prominences, and the role of these structures in flares and coronal mass
ejections.
This work is supported by NASA via the AIA contract to Lockheed Martin (subcontract
SP02D4301R).