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 0.2 arcsecRHESSI 2.3 arcsecSOT exposure: 0.03sRHESSI image: >4s

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Hinode/SOT G band (430 nm): 0.2 arcsec resolution

yellow contours: G band image convolved with RHESSI resolutionlevels: 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 resolutionlevels: 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 resolutionlevels: 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 beamlevels: 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 E0=10 (25) keV:

very large energy deposit rate: 8 (2) x1012 erg s-1 cm-2

This is more than enough to heat entire column density

Very large beam densities similar to coronal densities!2x109 – 4x1010 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?