Solar Cycle 24 Group F
From RHESSI Wiki
Tuesday 9th Dec
Introduction 14:30 - 16:00
STERLING Earliest phases of solar eruptions
preflare phase & trigger mechanism for filaments as tracer of B field, slow rise -> flare + fast rise
few (12) example event studied. 2 may 2007, TRACE & HINODE, good example.
filaments undergo slow rise (few km/s), then fast. the slow rise is linear then flare at start of fast eruption. could be some signatures of 'breakout'
dimmings - local (near neutral line) or remote (associated with breakout?)
QUESTIONS ARISING:
how common is a slow rise?
what triggers slow & fast rise phases?
where to go from here? Clearly Hinode and SECCHI 171 2 min cadence? so synoptic data modes are fine for this project?
ATRILL Coronal waves and dimmings
EIT waves map the CME footpoints? Angelos -mixing lateral mass expansion & wave? Atrill - the expansion of CME stops when wave stops.
Explains the brightnenings at the CME legs
WD - Tunnelling of waves into coronal hole?
Dimmings: could be evacuation or cooling also agree with deep core and secondary dimmings
Mass measurements from plasma outflows?
Angelos: No brightenings in 304, so not reconnection? McAteer: reflection and refraction problem?
Attril: does not mean there is no wave, the CME footpoints could cause a wave?
why/how do CD disappear while magnetic connectivity of the CME ejecta to Sun is maintained? recovery can be due to Interchange reconnection.
reconnection rate at same speed as the wave? 0.1 X 0.2 alfven speed - too low?
expansion of cme flanks should correspond with eit wave speed.
McAteer
Atrill
Steed
Howard
Events 17:00-18:30