xu et al., apj 607, l131, 2004: or, how do flare footpoints work? first flare observations in the...
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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)
Left: speckle WL preflare; right, flare image at 1.56
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20:52:1520:42:4620:39:45
Nice Sa”m Krucker RHESSI images
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
Nitty-gritty of the observations
• Dunn Solar Telescope @ near diffraction limit, high-order AO
• 10242 NIR array, 5nm passband @ 1.56, 13 ms sampling, 91 arc s FOV
• IR has better seeing (-6/5) but should have lower contrast
Ancient history! Ohki & Hudson, 1975
Blue: RHESSI 50-100 keV; Red: IR
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Bruzek, 1964
Maltby models for sunspot umbraand particle ranges
Flare spectroscopy: Shoji & Kurokawa 1995
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?