Imaging with subcollimator 1. Dec 6, 2006 white light flare Hinode/SOT image during the main HXR peak! 880 -870 -860 - 850 -840 -830 - 820 SOT resolution.

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Presentation transcript:

Imaging with subcollimator 1

Dec 6, 2006 white light flare Hinode/SOT image during the main HXR peak! SOT resolution 0.2 arcsec RHESSI 2.3 arcsec SOT exposure: 0.03s RHESSI image: >4s

Hinode/SOT G band (430 nm): 0.2 arcsec resolution yellow contours: G band image convolved with RHESSI resolution levels: 15, 30, 45, 60, 75, 90 %

Hinode/SOT G band (430 nm) CLEAN image (subcoll. 1 and up) yellow contours: G band image convolved with RHESSI resolution levels: 15, 30, 45, 60, 75, 90 %

Hinode/SOT G band (430 nm) CLEAN image (subcoll. 1 and up) yellow contours: G band image convolved with RHESSI resolution levels: 15, 30, 45, 60, 75, 90 %

Hinode/SOT G band (430 nm) CLEAN image (subcoll. 1 and up) yellow contours: G band image convolved with RHESSI clean beam levels: 15, 30, 45, 60, 75, 90 %

Cross-section of main footpoint G band emission is clearly resolved: 1.6” ____ G band ---- PSF

Cross-section of main footpoint G band emission is clearly resolved: 1.6” HXR unresolved ____ G band ---- PSF ____ G band ---- PSF ____ HXR ---- PSF

Cross-section of main footpoint G band emission is clearly resolved: 1.6” FWHM HXR unresolved: 3.0” FWHM Convolved G band: 3.4” FWHM ____ G band ---- PSF ____ G band ---- PSF ____ HXR ---- PSF …. G band + RHSI PSF

If HXR size= WL size Area of 1.6”x1.6” & THICK target assumption with E 0 =10 (25) keV: very large energy deposit rate: 8 (2) x10 12 erg s -1 cm -2 This is more than enough to heat entire column density Very large beam densities similar to coronal densities! 2x10 9 – 4x10 10 cm -3  beam models are in trouble! Other ideas should be studied as well: electron acceleration in footpoints (e.g. Fletcher & Hudson 2008)? purely non-thermal bubble of electrons?