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</o:shapelayout></xml><![endif]--></head><body lang=EN-US link=blue vlink=purple><div class=WordSection1><p class=MsoNormal><span style='color:#1F497D'>Hi Joan,<o:p></o:p></span></p><p class=MsoNormal><span style='color:#1F497D'><o:p> </o:p></span></p><p class=MsoNormal><span style='color:#1F497D'> Thanks! Looks like a nice paper, and I look forward to reading it. I have a quick comment based on the abstract. Low-frequency nanoflare models predict that the 10 MK emission should be very faint, in part because the emission measure is expected to be small and in part because of nonequilibrium ionization. The actual emission measure, though small, may be much larger than what one infers from data by assuming equilibrium ionization. Steve and I give some specifics in our 2011 paper (ApJ Supp, 194, 26). Fabio has also done some work on this.<o:p></o:p></span></p><p class=MsoNormal><span style='color:#1F497D'><o:p> </o:p></span></p><p class=MsoNormal><span style='color:#1F497D'>Cheers,<o:p></o:p></span></p><p class=MsoNormal><span style='color:#1F497D'>Jim<o:p></o:p></span></p><p class=MsoNormal><span style='color:#1F497D'><o:p> </o:p></span></p><div style='border:none;border-left:solid blue 1.5pt;padding:0in 0in 0in 4.0pt'><div><div style='border:none;border-top:solid #B5C4DF 1.0pt;padding:3.0pt 0in 0in 0in'><p class=MsoNormal><b><span style='font-size:10.0pt;font-family:"Tahoma","sans-serif"'>From:</span></b><span style='font-size:10.0pt;font-family:"Tahoma","sans-serif"'> Loops [mailto:loops-bounces@solar.physics.montana.edu] <b>On Behalf Of </b>Joan T Schmelz (jschmelz)<br><b>Sent:</b> Friday, January 25, 2013 11:13 AM<br><b>To:</b> Loops@solar.physics.montana.edu<br><b>Subject:</b> [Loops] New Loop Paper<o:p></o:p></span></p></div></div><p class=MsoNormal><o:p> </o:p></p><p class=MsoNormal>Dear Colleagues,<o:p></o:p></p><p class=MsoNormal><o:p> </o:p></p><p class=MsoNormal>The following paper on EIS+XRT coronal loop DEM analysis has just been published in ApJ:<o:p></o:p></p><p class=MsoNormal><o:p> </o:p></p><p class=MsoNormal>Deeper by the Dozen: Understanding the Cross-Field Temperature Distributions of Coronal Loops<o:p></o:p></p><p class=MsoNormal>by Schmelz, J.T., Pathak, S. Jenkins, B.S., Worley, B.T. 2013, ApJ, 764, 53.<o:p></o:p></p><p class=MsoNormal><o:p> </o:p></p><p class=MsoNormal><a href="https://umdrive.memphis.edu/jschmelz/public/Loops/Dozen_SchmelzEtAl_2013.pdf">https://umdrive.memphis.edu/jschmelz/public/Loops/Dozen_SchmelzEtAl_2013.pdf</a><o:p></o:p></p><p class=MsoNormal><o:p> </o:p></p><p class=MsoNormal>Abstract: Spectroscopic analysis of coronal loops has revealed a variety of cross-field temperature distributions. Some loops appear to be isothermal while others require multithermal plasma. The EUV Imaging Spectrometer on Hinode has the spatial resolution and temperature coverage required for differential emission measure (DEM) analysis of coronal loops. Our results also use data from the X-Ray Telescope on Hinode as a high-temperature constraint. Of our 12 loops, two were post-flare loops with broad temperature distributions, two were narrow but not quite isothermal, and the remaining eight were in the mid range. We consider our DEM methods to be a significant advance over previous work, and it is also reassuring to learn that our findings are consistent with results available in the literature. For the quiescent loops analyzed here, 10 MK plasma, a signature of nanoflares, appears to be absent at a level of approximately two orders of magnitude down from the DEM peak. We find some evidence that warmer loops require broader DEMs. The cross-field temperatures obtained here cannot be modeled as single flux tubes. Rather, the observed loop must be composed of several or many unresolved strands. The plasma contained in each of these strands could be cooling at different rates, contributing to the multithermal nature of the observed loop pixels. An important implication of our DEM results involves observations from future instruments. Once solar telescopes can truly resolve X-ray and EUV coronal structures, these images would have to reveal the loop substructure implied by our multithermal results.<o:p></o:p></p><p class=MsoNormal><o:p> </o:p></p><p class=MsoNormal>Regards,<o:p></o:p></p><p class=MsoNormal>Joan<o:p></o:p></p><p class=MsoNormal><o:p> </o:p></p><p class=MsoNormal><o:p> </o:p></p></div></div></body></html>