Long-Term Solar Variability (LSV) Section
Coronal and Heliospheric Evolution
The magnetic field in the Sun's atmosphere continuously evolves through processes of emergence, diffusion, and reconnection, resulting in ongoing reorganizations of the global coronal and heliospheric magnetic morphology, as well as in the slow buildup of magnetic energy in twisted or sheared magnetic fields.
HAO scientists undertake observational and theoretical studies of the build-up of magnetic energy and other slow (month-to-year timescale) changes in coronal and heliospheric magnetic fields. Read More »
Currently, HAO scientists are conducting observational studies and forward modeling of coronal prominences and cavities to better understand the precursor magnetic structure and triggers of coronal mass ejections. Read More »
See Profiles in Science pages for Giuliana de Toma,and Sarah Gibson.