WORKING GROUP C: ENERGETIC PARTICLE OBSERVATIONS

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WORKING GROUP C ENERGETIC PARTICLE
OBSERVATIONS

• Co-Chairs Klecker, Kunow
• SUMMARY FROM WORKSHOP 1
• Observations
• Questions
• Specific Questions for Theory Group
• Event List

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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

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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?

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QUESTIONS-2

• Why are all particle events gt 50 MeV flare
  associated?
• (related to event size? shock acceleration?)
• Why arent 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?
• -gt 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?

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QUESTIONS-3

• Are ionic charge states of energetic particles (
  0.05-1 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

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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

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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?

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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)

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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.

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COMMON EVENT LIST