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THE IMPULSIVE X-RAY RESPONSE IN FLARE FOOTPOINTS. TOMASZ MROZEK WROCLAW UNIWERSITY ASTRONOMICAL INSTITUTE POLAND. OBSERVATIONS. Soft X-Ray Telescope(SXT) grazing incidence telescope AL12 BE119 Hard X-Ray Telescope(HXT) Fourier synthesis imager L 14-23 keV M1 23-33 keV
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THE IMPULSIVE X-RAY RESPONSE IN FLARE FOOTPOINTS TOMASZ MROZEK WROCLAW UNIWERSITY ASTRONOMICAL INSTITUTE POLAND
OBSERVATIONS Soft X-Ray Telescope(SXT) grazing incidence telescope AL12 BE119 Hard X-Ray Telescope(HXT) Fourier synthesis imager L 14-23 keV M1 23-33 keV M2 33-53 keV H 53-93 keV
OBSERVATIONAL CHARACTERISTICS • Duration time • Time profile characteristics • SXR/HXR delay • Relative duration
A „typical” impulsive SXR brightening: 1. Lasts about 0.5-1min. 2. Has symmetrical time profile. 3. The diameter is about 2-8 SXT pixels. 4. Temperature below 10 MK and electron density below 1011 cm-3. 5. Relative brightness below 0.1. 6. Lasts several times longer than HXR burst. 7. Shows a delay in comparision with the HXR burst. 8. Delay has Poisson distribution (τ = 35 s).
CONCLUSIONS • Thedescribedcharacteristicsshould help to distinguishthe • impulsive SXR brighteningsfromothermorphologicalfeatures • and should help inthemodelling of theimpulsivephase. • A generallygoodspatial and temporalcorrelationbetween • impulsive SXR brightenings and HXR burstsstronglysuggests • the same origin : non-thermal electronbeams. • Thestrongcorrelationbetweenthe SXR and HXR responsecan • be considered to be a proof thatimpulsive SXR brightenings • aredirectlyresponsible for theNeuperteffect. • A steeper energy spectrum of HXR photonscauses a higher • relativeproductivity of SXRs. • Thereis a correlationbetweentheenergies : thetotal, • time-integrated energy deposited by non-thermal electrons • and themaximum thermal energy containedintheplasma • heated by thoseparticles.