Page tree
Skip to end of metadata
Go to start of metadata

You are viewing an old version of this page. View the current version.

Compare with Current View Page History

« Previous Version 13 Next » Prompt events:

  • 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)?


In X-ray literature "prompt event" is defined as an event where the estimated release time of the electrons that are later seen at 1 AU agrees with the hard X-ray flare peak time within the uncertainty of a few minutes. (YZ: I don't see any difference with the "impulsive" events term used in energetic particles papers, but the correspondence is not 1-1, see below).

Also the spectral shapes of the in situ observed electron spectrum and hard X-ray photo spectrum are statistically correlated. This suggests that a common accelerator produces both the hard X-ray emitting electrons and the escaping electrons (Droege 1996, Krucker et al. 2007). However the observed correlation does not agree with the prediction of the thick-target model (Brown 1971) that would be expected for footpoint emission. This is currently not understood.

Hard X-ray imaging of the solar source region of prompt events often reveals three sources. Frequently jets are observed in EUV and soft X-rays that appear to emanate from the hard X-ray sources. This geometry is similar to that of interchange reconnection models where closed field lines reconnect with open fields. The jet indicates the direction of open field lines along which electrons escape. Prompt events are well correlated with the occurence of 3He rich SEP events.

However, arrival time studies of ions seen at 1 AU suggest a delayed release of the ions relative to electrons, at least when assuming scatter-free transport. This is rather puzzling as it suggests a different accelerator for electrons and ions despite the closely connected occurrence. However, electrons and ions could still be released simultaneously with propagation effects explaining the observed delays.

This objective is about exploring if the comparative delay is real or due to propagation effects. It should be studied in different heliocentric distances and hopefully near the perihelion in order to better establish the nature of the flare region (with STIX & EUI).


Complete set of observations is required: STIX, EUI, RPW + ground based radio observations (good to have). That will allow to study the magnetic structures along which flare-accelerated particles escape into interplanetary space. 



Required observations:

  • SWASWA Normal Mode, several hours, perihelion, other instruments: RPW, MAG, EPD, STIX.
  • MAGMAG Normal Mode
  • RPW
  • SoloHI: Contribute (mode: shock+synoptic), no min. obs time, all distances, w/EUI-STIX-METIS.
  • EUIEUI Synoptic mode (S). EUI FD 174, 304, cadence 10 min. EUI HR 174 and Ly-alpha, cadence 1 min for 30 min before and during X-ray peak.
  • 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.
  • STIX


  • 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:Other instruments: PHI, EUI, STIX, SoloHI, MAG, SWA, EPD, RPW.
      • 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.


  • Several hours.

Other constraints:

  • Perihelion.
  • No labels