A flare compilation Lots of people including Louise Harra, Lidia van Driel Gesztelyi, Chris Goff, Sarah Matthews, Len Culhane, Cristina Mandrini, Pascal.

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Presentation transcript:

A flare compilation Lots of people including Louise Harra, Lidia van Driel Gesztelyi, Chris Goff, Sarah Matthews, Len Culhane, Cristina Mandrini, Pascal Demoulin, Lyndsay Fletcher

15 Jul 02 – two filament eruptions and a couple of CMEs

Spectroscopic evidence for break-out In contrast to the standard model reconnection starts high in the corona. Evidence has been found in the form of remote brightenings (and flows) prior to the impulsive phase. Gary and Moore., 2004, Harra et al Sterling and Moore

Pre-eruption stage Following filament eruption Spatially resolved evaporation has been observed in various cases now e.g.Brosius and Phillips (2004) with velocities 10s km/s and del Zanna et al (2005) with velocities reaching 140 km/s. Harra et al., 2005

SOHO/CDS slit TRACE EUV image Fe XIX Doppler velocity V l < 0 V l > 0 Time  13:00 15:00 Flare loops Flux rope Fe XIX intensity Flux rope Flare loops Time  PositionPosition CDS Synthetic slit image made of TRACE data SOHO/CDS observations

disc centre view rotated and tilted to event location view tilted to show arcade orientation Magnetic field lines extrapolated in the linear force-free approximation (  =0.015 Mm -1 ) using a SOHO/MDI magnetic field map on 14 April in order to determine the 3-D spatial orientation of the flare loop and deduce the direction of plasma flows from the Doppler data. flare time Magnetic modelling

V l >0 V l <0 time p o si ti o n Fe XIX Doppler velocity S leg points away from us - Red-shifted in CDS N leg points towards us - Blue-shifted in CDS Plasma is flowing down along both legs of the flare loops Combining modelling results with CDS Doppler shift

RHESSI keV contours (made with PIXON) over TRACE images show a rising coronal X-ray source. Images made in the 5-10 keV and keV ranges show very similar motion pattern. RHESSI observations: Moving (rising) coronal X-ray source Looptop sourceRising coronal source v≈60 km/s

Erupting filament (TRACE) Rising X-ray source (RHESSI) Height - time plot of the lifting flux rope as seen by TRACE. The cross in the red circle represents the leading edge of the flux rope as seen by CDS. Below the best-fit lines are data points from the coronal hard X-ray source. HXR RHESSI light curve between 5-50 keV. Height-time plots - low corona CDS observation

Height-time plot of lifting filament in TRACE images Height-time plot of CME leading and trailing edges in LASCO/C2 images An exponential growth makes the link between the two curves, while neither the linear nor the polynomial fit can reach the required height by the C2 appearance time of the CME. Height-time plots - TRACE & C2 v CME ~ 120 km s -1

V l >0 V l <0 Flux rope SOHO/CDS slit TRACE EUV image time p o si ti o n Fe XIX Doppler velocity Cooling loops +   magnetic extrapolation  3-D flare loop orientation New evidence for flux rope structure of an erupting filament Linking a rising RHESSI coronal source to the erupting filament New evidence for exponential growth of CMEs in the low corona - result of kink instability? Results consistent with down-flows of hot plasma along both loop legs. RHESSI source ~60 km/s LASCO/C2 v~120 km/s Blabla blabla Blab l Height-time plot, high corona TRACE LASCO/C2 Contour: RHESSI keV EUV flux rope v~45-75 km/s Exponential growth Height-time plot, low corona v~60 km/s A&A 434, 761 (2005)