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SUMMARY:Alfven wave phase-mixing in flows: why over-dense solar coronal op
 en magnetic field structures are cool? - David Tsiklauri (Queen Mary)
DTSTART:20161031T160000Z
DTEND:20161031T170000Z
UID:TALK67011@talks.cam.ac.uk
CONTACT:Robert Teed
DESCRIPTION:We include the effect of plasma flow in Alfvén wave (AW) damp
 ing via phase mixing and to explore the observational implications. We app
 ly our findings to addressing the question why over-dense solar coronal op
 en magnetic field structures (OMFS) are cooler than the background plasma.
  Observations show that the over-dense OMFS (e.g. solar coronal polar plum
 es) are cooler than surrounding plasma and that\, in these structures\, Do
 ppler line-broadening is consistent with bulk plasma motions\, such as AW.
  If over-dense solar coronal OMFS are heated by AW damping via phase-mixin
 g\, we show that\, co-directional with AW\, plasma flow in them reduces th
 e phase-mixing induced-heating\, thus providing an explanation of why they
  appear cooler than the background. Recent advances in solar flare radio e
 mission mechanisms modelling will be also very briefly discussed.
LOCATION:MR14\,  Centre for Mathematical Sciences\, Wilberforce Road\, Cam
 bridge
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