Abstract
Alan Title
The Magnetic Field and its Effects on the Solar Atmosphere in High Resolution
The Sun’s magnetic field is produced throughout the solar interior; it emerges and is dispersed by surface and subsurface flows, and then expands above the surface to dominate the structure of the corona. To resolve the effects of the magnetic field it is necessary to image the interior and measure its rotation and flow systems; track the responses of the magnetic fields to flows in the surface; and to follow the evolution of structures in the corona. Because the Sun is dynamic both high spatial and temporal resolution are essential. Because the Sun’s magnetic field effects encompass the entire spherical exterior, the entire surface and outer atmosphere must be mapped. And because the magnetic field is cyclic high-resolution observations must be maintained over multiple cycles.
This talk will illustrate solar phenomena with a sampling of the highest resolution images and movies of the photosphere, chromosphere, and corona. Many of the observations are both strikingly beautiful and surprising in their complexity. Surprising observations are the reason science is so exciting. Each new surprise drives new approaches, insights, and understanding. It is not discouraging that many complex interactions are occurring in the Sun it is exciting, challenging, and important to all of physics and astrophysics.
