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  • How shocks can accelerate electrons to relativistic energies (never observed for shocks near 1 AU)? Is a more energetic seed population necessary?



Required observations:

  • SWASWA Normal Mode, several hours, perihelion, other instruments: RPW, MAG, EPD.
  • MAGMAG Normal Mode
  • EPD: All sensors: spectra, composition, fluxes, directional information, together with IS instruments. Solar source identification by RS instruments (full disk imaging). Also coordinated multi-s/c SEP observation campaigns with SPP & other missions.
  • RPW
  • and some good theorists!
  • Several hours.

Other constraints:

  • Perihelion.

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