184.108.40.206 How are so many electrons accelerated on such short time scales to explain the observed hard X-ray fluxes?
- Understand the transport of electrons from the coronal acceleration site down to the hard X-ray footpoints (Miller et al., 1997; Önel et al., 2007; Battaglia and Benz, 2007).
- Understand effects of non-uniform plasma ionisation (Kontar et al., 2003), return current (Zharkova and Gordovskyy, 2006), and beam-plasma interaction via various plasma waves (Kontar, 2001).
- Partially limb-occulted flare observations: provide unique information about the suprathermal electrons closest to the site in the corona where their acceleration is believed to occur (Krucker and Lin, 2008).
- Study coronal phenomena in hard X-rays associated with CMEs:
- Highly occulted events associated with fast backside CMEs (Krucker et al., 2007), non-thermal bremsstrahlung.
- Produced by flare-accelerated energetic electrons (>10 keV) trapped in magnetic structures related to the CME or
- Accelerated in CME current sheets or other coronal magnetic restructuring related to the CME.
- Explore the consequences of particle acceleration by Alfvén waves created by the magnetic reconfiguration during magnetic reconnection (Fletcher & Hudson, 2008).
- SoloHI: Contribute (mode: shock+synoptic), no min. obs time, all distances, w/EUI-STIX-METIS.