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3.3.1 What are the properties and distribution of suprathermal seed populations?

3.3.1.1 Characterization of the suprathermal population

  • Solar wind ions
  • Flare populations
  • Gradual SEP events
  • Pickup ions
  • Other particle populations

3.3.1.2 Characterize the suprathermal elemental and charge-state composition as a function of energy (Fisk and Gloeckler, 2007), time (Desai et al., 2006a,b), and location.

 

3.3.1.3 Role of shocks in generating SEPs: comparison between the composition of suprathermal ions near the shocks and that of energetic particles. Distinction for quasi-perpendicular and quasi-parallel shocks. Spectroscopic observations of CME shocks’ line profiles. Visible light and UV observations of shocks in the inner corona.

 

 

Required observations:

  • SWASWA Triggered ModeSWA Burst Mode (Scheduled), 5 min captures of shock near perihelion or several days during SEP evolution in normal mode, other instruments: ALL.
  • SoloHI: Contribute (mode: shock+synoptic), no min. obs time, all distances, w/ in situ, METIS.
  • All instruments.

Duration:

  • 5 min captures of shock near perihelion or several days during SEP evolution in normal mode.

Other constraints:

  • Near perihelion.

 

 

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