Solar Cycle 24 Group F

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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

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