CME Workshop Elmau, Feb , WORKING GROUP C: ENERGETIC PARTICLE OBSERVATIONS Co-Chairs: Klecker, Kunow SUMMARY FROM WORKSHOP 1 Observations Questions Specific Questions for Theory Group Event List

CME Workshop Elmau, Feb , OBSERVATIONS Intensity-time profiles Elemental, Isotopic, Ionic Charge Composition Energy Spectra Q/M-related compositional systematics Relation to observations of CMEs at the Sun Relation to observation of IP Shocks Energetic particle observations in CMEs and CIRs; differences and similarities Energetic particle observations in CMEs and Impulsive Events; differences and similarities

CME Workshop Elmau, Feb , QUESTIONS-1 Are there two classes of CMEs / gradual particle events? – (related to (1) CMEs accelerating and (2) CMEs starting with high velocity. Are all the particles created at the shock driven by the CME? (2-shock question, any particles from the first shock?) What are EIT waves? (Evidence for a shock?) Why are meter wavelength type II bursts nearly always present and yet die out within about 10 solar radii? What are SA events and and are they forecasters for proton acceleration at the Sun?

CME Workshop Elmau, Feb , QUESTIONS-2 Why are all particle events > 50 MeV flare associated? – (related to event size? shock acceleration?) Why aren’t different types of bidirectional flows co-spatial? (differences of spatial distribution between fast (e, high energy p) and slow (low energy p) particles) What are the radial speeds of CMEs near the Sun? (projection effect? – -> probably small ~ 15%) Is there a non-radial component in the expansion of CMEs? Is the replenishment of mass after CME lift-off a problem? What is the time scale?

CME Workshop Elmau, Feb , QUESTIONS-3 Are ionic charge states of energetic particles (~ MeV/nuc) similar or different from SW ionic charge states? (does Q/M dependent acceleration change the ionic charge distribution?) Energy dependent ionic charge states – is stripping at low coronal altitudes the only answer or could Q/M dependent acceleration / injection effects contribute? What determines the Q/M dependent systematics of elemental and isotopic abundances in gradual events? – (elemental and isotopic abundance variations ordered by Q/M, - NOT Q/M dependent resonant effects as observed in 3He/heavy ion-rich events) New results / papers since 2002: Charge Composition: Möbius et al., 2001, Klecker et al., 2001; Popecki et al., 2001;

CME Workshop Elmau, Feb , QUESTIONS-4 What determines spectra in the late stages (decay phase) of particle events? (isotropy, „universal“ spectra) Comparison of accelerated particles at the shock and in the post-shock region with upstream waves and downstream turbulence? How can we use of different source populations to explore acceleration / injection effects (e.g. Pickup He+). High 3He (3He/4He~ 0.01) abundances in gradual / CME-related events: mixed events or acceleration of a pre-existing population of energetic particles from previous Impulsive Events? What is the origin of the quiet-time component of energetic particles? New results / papers since 2000: Mason et al., 2000, 2002;

CME Workshop Elmau, Feb , QUESTIONS-5 The velocity distribution of CMEs in Solar Minimum and Solar Maximum is similar, however, Gradual SEPs are different. Why? The effect of CMEs on GCR modulation during solar minimum and maximum is different. Why? 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). What can solar energetic particles tell us about the large scale topology of CMEs and the global structure of the corona?

CME Workshop Elmau, Feb , QUESTIONS FOR THEORY GROUP-1 Are M/Q-dependent effects from shock acceleration (Injection? Acceleration? Transport?) compatible with – M/Q-dependent systematics in elemental and isotopic abundances – differences between solar wind and energetic particle ionic charge states – can these effects contribute to the energy dependence of – Ionic charge states Are there alternatives to shock acceleration in the inner helio-sphere in gradual events (as e.g. transit time damping used to model the suprathermal tails of pickup ion distributions in CIRs as seen with Ulysses)

CME Workshop Elmau, Feb , QUESTIONS FOR THEORY GROUP-2 How can we understand the observed correlation between Heavy Ion abundances and ionic charge states in Gradual and Impulsive Events Do we understand intensities and spectra in the decay phase of IP-shock / CME related solar energetic particle events.

CME Workshop Elmau, Feb , COMMON EVENT LIST