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WG4 Multi-wavelength Correlative Studies Group Members. Marina BATTAGLIA Cristina CHIFOR Brian DENNIS Martin FIVIAN Lyndsay FLETCHER Iain HANNAH Hugh HUDSON Haisheng JI Joe KHAN Säm Krucker Helen MASON Ryan MILLIGAN Manuela TEMMER Mikko VÄÄNÄNEN Lidia van DRIEL-GESZTELYI
Manuela TEMMERMikko VÄÄNÄNEN
Lidia van DRIEL-GESZTELYI
11:00 – 13:00 RHESSI Thermal / low energy / multi-l spectroscopy
14:30 – 18:00 Footpoints Part I
09:00 – 10:30 Coronal sources, joint with WG3
11:00 – 13:00 Footpoints Part II
14:30 – 16:00 Joint session with WG2 – Oct 28th event
16:30 – 18:00 Joint with WG5 – soft-hard-soft, number problem, etc.
09:30 – 11:00 Energetics
Discrepancies could be due to: instrumental effects,
errors in atomic rates
Offpoint RHESSI from Sun to modulate QS signal and separate from background: noise limited or signal ?
XSM/RHESSI lightcurve 6-8kev
Brightenings parallel to flare ribbons were observed with RHESSI (Grigis + Benz)
Survey of brightenings associates with erupting filaments in EIT shows many examples of brightenings along arcade footpoints
Slow speeds correspond to slow eruptions
Plasma velocities observed with CDS during impulsive phase of 2 flares
(17-Jan-2005 X3.8 flare)
RHESSI HXR sources occur only along certain parts of the Ha ribbon edges
Higher local reconnection rates (factor 5-10) at these sites
HXR sources tend to avoid strongest magnetic fields and umbrae.
Almost vertical inclination of field lines does not favour reconnection there?
Peculiar motions/spatial jumps of HXR sources?
Reconnection rises through field lines of lines of different altitudes, with distant footpoint locations
LV 25 arcsec
LV 100 arcsec
Red contour: 30-50 keV
Blue contour: 3-10 keV
Green contour: 34GHz
The distance and velocity between the two Ha kernels
The distance between the two HXR FPs
The ‘height’ of the HXR loop top source
The flare shear time profile
The rate of change of flare shear
RHESSI imaging - spectroscopy finds soft-hard-soft behavior in the coronal source of several flares might be a feature of the accelerator and not a transport effect
Time evolution of spectral index
and non-thermal flux at 35 keV
of coronal hard X-ray spectra
Reconnection Outflow Termination Shock (TS)
SDA at the TS can reproduce required electron fluxes & power
Is the ‘termination shock’ suggested by Warmuth et al a standing shock at all?
Moreton/coronal wave seen in radio
Dotted line: Edge of Ha Moreton wave
Flux – spectral index correlation (“SHS”) – presentation by Grigis on a transit-time damping model
Electron total numbers, fluxes, and predicted/observed response of atmosphere – discussion by all
Presentation by Pick on Type III bursts associated with compressing edge of a CME – new theoretical challenge (see Steven’s presentation)
Fe XIX Doppler velocity
van Driel/Goff et al
1 px = 0.5” ~ 300km