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3.1.2.5 Prompt events:

  • In-situ observed electron spectrum and hard X-ray photon spectrum correlation:
    • Explore why there is no agreement with the prediction of the thick-target model (Brown, 1971) that would be expected for footpoint emission.
  • Arrival time of ions at 1 AU suggest a delayed release of the ions relative to the electrons (Wang et al., 2005), is this due to:
    • Different accelerators for electrons and ions or
    • Propagation effects (turbulence, diffusion, magnetic connectivity)?

 

Required observations:

  • SWASWA Normal Mode, several hours, perihelion, other instruments: RPW, MAG, EPD, STIX.
  • MAGMAG Normal Mode
  • SoloHI: Contribute (mode: shock+synoptic), no min. obs time, all distances, w/EUI-STIX-METIS.
  • 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.

 

  • METIS: Measurement of coronal outflow velocity and density in corona to identify the shock front. Measurement of shock passage timing relative to the flare occurrence.
    • Products:
      • CME velocity maps 
      • CME density maps 
      • CME directionality
      • CME flag
    • Modes:
      • GLOBAL (before the event, if possible), min. obs time 2 hr, data volume ≤ 300 Mb.
      • CMEOBS, starts after CME flag rise, min. obs time 1 hr (high cadence, 1 min), data volume ~ 2.137 Gb.
      • GLOBAL (after the event), min. obs time 2 hr, data volume ≤ 300 Mb.
    • Other instruments: PHI, EUI, STIX, SoloHI, MAG, SWA, EPD, RPW.

Duration:

  • Several hours.

Other constraints:

  • Perihelion.
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