WG 1: CME Initiation
To address these important CME initiation issues, we will concentrate on the role played by the vector magnetic field and the surface velocity fields in the build-up to a CME.
- What aspects of the photospheric and coronal evolution are necessary and/or sufficient for an eruption to occur?
- Is magnetic complexity crucial to CME production?
- What photospheric motions, or emergence/submergence of flux are required for a CME to be initiated?
WG1-2: Modeling the Evolution of Photospheric and Coronal Magnetic Fields
- Can we utilize the models of the evolutionary behavior of the surface magnetic fields to predict solar wind variability?
- How good are potential field models for large-scale field connectivity and interplanetary connections?
WG2: Interplanetary
This session will focus on the modeling and prediction of the ambient solar wind. The goals of this session are to establish how well we can do using our current solar wind models, highlighting both their strengths and limitations, and to have vigorous, open discussion on what can be done to further improve the modeling and prediction of the ambient solar wind.
WG2-3: Suprathermal Particles
The focus of this session is on the nature and implications of suprathermal particle signatures. We plan to discuss a broad range of issues such as ion and electron counterstreaming, flux dropouts, variable properties of electrons with energy, and transport. We will evaluate their usefulness for discerning disconnected fields and implications for magnetic connection of CMEs to the Sun.
WG3: SEPs
This session will focus on recent attempts to understand the observed spectral and compositional variability in energetic particles at CME-driven shocks, both near-Sun and in situ. The effects of shock-geometry, near-shock wave-particle interactions, seed population and injection processes will be investigated. The session will also address recent observational challenges for our understanding of ion acceleration at flare sites.
WG1-3: The Role of Energetic Particles
This joint topic will focus on the acceleration and transport of energetic particles and what we can learn about the relationship between SEP events, CMEs, and flares.
- What, if any, is the relationship between the particles produced close to the Sun and those seen in interplanetary space?
- How does the field topology in the corona influence the variability observed in SEP events?
- Can flare-accelerated particles provide a seed population for further acceleration at a CME–driven shock front?
- Can we determine where shocks become established in the solar corona and how they evolve as they move outward through the corona?