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Xu et al., ApJ 607, L131, 2004: or, how do flare footpoints work? First flare observations in the infrared 1.56 nominally is as deep as deep can be (the opacity minimum) Lucky to get an X10 flare (Oct. 29, 2003; good RHESSI observations)
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Left: speckle WL preflare; right, flare image at 1.56
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20:52:15 20:42:4620:39:45 Nice Sa”m Krucker RHESSI images
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Footpoints and ribbons Anchor flaring coronal loops and interface with the mass reservoir there Traditional modeling in 1D radiation hydro approximation Hard X-ray (beam?) and UV-O-IR (deep atmosphere?) morphology significantly different
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Nitty-gritty of the observations Dunn Solar Telescope @ near diffraction limit, high-order AO 1024 2 NIR array, 5nm passband @ 1.56 , 13 ms sampling, 91 arc s FOV IR has better seeing ( -6/5 ) but should have lower contrast
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Ancient history! Ohki & Hudson, 1975
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Blue: RHESSI 50-100 keV; Red: IR
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Bruzek, 1964
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Maltby models for sunspot umbra and particle ranges
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Flare spectroscopy: Shoji & Kurokawa 1995
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Annotated conclusions Backwarming response (theory somewhat confused) V x B @ 45 V/cm, but is this really a relevant E? Weak photospheric lines in the passband - do they contribute?
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