1. CME Workshop Elmau, Feb 6 - 12, 20031 WORKING GROUP C: ENERGETIC PARTICLE OBSERVATIONS Co-Chairs: Klecker, Kunow SUMMARY FROM SESSION 1B Discussion of Questions from last Workshop Selection of Topics for Further Discussion + Presentations Selection of Topics to be Transferred to other WG

2. CME Workshop Elmau, Feb 6 - 12, 20032 Topics for Further Discussion + Presentations (P) in WG C - 1 How does the timing of e and p injection as derived from interplanetary measurements compare with the event onsets observed at the Sun (e.g. CME, type II, type III, flare). P: p-, e - onset and radio signatures (Klein+Posner) P: Observations at high latitudes (Ulysses) (Dalla) Shock and / or Flare Acceleration in Large SEP Events Large events with E> 50 MeV p flux are flare related Large events with high Fe/O ratio, high Fe charge states at > 20 MeV/n P: Correlation of Type III-l with p; Anti-correlation of high Fe/O with Shock transit-time (Cane)

3. CME Workshop Elmau, Feb 6 - 12, 20033 Topics for Further Discussion + Presentations (P) in WG C - 2 P: 3 He observation in large events (Klein) P: The May 7, 2001 event as seen by ACE and Ulysses (CME, no flare) (Simnet) P: Electron Acceleration (Simnet) P: Multiple shocks / CMEs and particle acceleration (Gopalswamy) Energy dependent ionic charge states – stripping at low coronal altitudes? Q/M dependent acceleration / injection effects? Transition from Solar Wind source (low energy) to ‘flare’ source (high energy) - > case studies Comparison of accelerated particles at the shock and in the post-shock region with upstream waves and downstream turbulence. P: Case studies with negative result (no waves observed) (Lario)?

4. CME Workshop Elmau, Feb 6 - 12, 20034 Topics for Further Discussion + Presentations (P) in WG C - 3 How can we use different source populations to explore acceleration / injection effects (e.g. SW source vs. Pickup He + ). P: Suprathermal He + observations in CMEs / IP shocks(Kucharek) Particle Propagation P: Study of decay time profiles - spectra in decay phase (Kecskemety) P: Evidence for perpendicular diffusion in large events. (Cane) The quiet-time component of energetic particles (e and ions). P: Quit-time ion observations (Kecskemety?) Extension of Event List from CME Workshop 1

5. CME Workshop Elmau, Feb 6 - 12, 20035 Questions Proposed to Transfer to other WG - 1 Transfer to What are EIT waves? (Evidence for a shock?)F Why are meter wavelength type II bursts nearly always presentF and yet die out within about 10 solar radii? The question of mass replenishment after CME lift-off. F Is there a non-radial component in the expansion of CMEs?G (important for particle acceleration, e.g. at CME flanks?) Do (1) CMEs starting with high velocities, (2) CMEs accelerating in the corona have different SEP signatures? G + C

6. CME Workshop Elmau, Feb 6 - 12, 20036 Questions Proposed to Transfer to other WG - 2 What can solar energetic particles tell us about the large scale topology of CMEs and the global structure of the corona? G + C ParticelObservations within CMEs (Lario) Perpendicular diffusion into CME (Rodriguez-Pacheco) The effect of CMEs on GCR modulation during solar minimum and maximum is different. Why? -> Differences in large scale topology, GMIRs. H

7. CME Workshop Elmau, Feb 6 - 12, 20037 QUESTIONS FOR DISCUSSION WITH WG D How do CMEs effect the energetic particle population Shock; trigger of acceleration at different location? M/Q-dependent systematics in elemental and isotopic abundances in CME / IP shock related SEP events (Injection? Acceleration? Transport?) How can we understand the observed correlation between Heavy Ion abundances and ionic charge states in Gradual and Impulsive Events Energy dependence of ionic charge states at ~ 0.020 - 20 MeV/nuc (M/Q dependent acceleration effect?, stripping at low altitudes?, flare particles at high energies?) Acceleration at IP / Coronal Shocks and Flare in the same event? Acceleration mechanism in flare. Energetics? Particle Numbers?

8. CME Workshop Elmau, Feb 6 - 12, 20038 OUR PROGRAM FOR TODAY 10:30Meeting WG C + D (+ continue C discussions) 15:00Meeting WG C + B (+ continue C discussions)