WG1: Solar Sources
Low coronal signatures of CMES
- What is the CME energy budget?
- What do the observations tell us about the partition of this energy budget into various forms (heating of plasma, acceleration of energetic particles, kinetic and gravitational energies of the CME)?
- What are the relationships between these forms of energy (is a fast CME always accompanied by significant heating of plasma in the low corona and acceleration of large numbers of particles)?
- When a massive prominence erupts, how much of the prominence mass is expelled with the CME?
- How do the observations of dimming relate to the magnetic geometry (e.g. do we see dimming regions at the base of an erupting flux rope)?
- What predictions can the various CME models make about dimmings, and how do these relate to the observations? When do dimming regions occur during the sequence of events (before or after the onset of the flare or CME)?
- How much of the mass loss in a CME can be accounted for by dimming (does all of the mass in a CME originate in the low corona, or does a significant fraction of the mass get swept up as the CME propagates outward)?
- Why do we not see dimming with every CME?
Understanding the corona from vector field measurements
- How are the coronal field models impacted by the forced lower boundary condition?
- How different are extrapolations based on chromospheric data from those base on photospheric data?
- How much energy is stored in the magnetic field? What isthe energy budget of a CME? How does the energy in the CME and flare compare to the energy contained in the magnetic field?
- What coronal fields and structures are implied by direct measurements of the coronal magnetic field?
WG1-2
Origin and evolution of the slow solar wind
- Where does the slow wind come from and what are the physical mechanisms that drive it?
- How does it differ from the fast wind?
WG3: Energetic Particles
Theory and Observations
What causes the increase in Fe/O with energy in some large SEP events?
WG1-3
Characteristics of impulsive SEP events and their solar origin
New measurements provide us with a great opportunity to test and constrain various particle acceleration models that are believed to operate during the so-called impulsive SEP events. This purpose of this session is to discuss key properties of such events in terms of their solar origins and current theoretical predictions.
WG1,2,3
Suprathermal-through-relativistic electrons during SEP events at 1 AU, their associated radio emissions and solar signatures
This session will investigate the relationship between electrons with energies ranging from hundreds of eV to tens of MeV and the associated radio emissions (e.g., Type II and III bursts) to identify their times of acceleration near the Sun and subsequent injection into the interplanetary medium
Extreme SEP Events, their solar origin and impact on geospace
This purpose of this session is to discuss similarities and differences between the well-documented extreme events of cycle 23 and those observed during previous solar cycles. The session will be focused on comprehensive discussions of the solar origin of such extreme events and their associated impacts on geospace.
Long-term effects of solar variability on the interplanetary magnetic field strength, the galactic cosmic radiation in the heliosphere, and Earth’s climate
Records can therefore be used to infer solar activity levels over the distant past and understand the relationship between the dynamic Sun and changes in the Earth’s climate. This session aims to characterize solar activity, the state of the heliosphere, and geomagnetic activity over the past ~1000 years.