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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='font-size:11.0pt;font-family:"Calibri","sans-serif";color:#1F497D'>Hi Viggo,<o:p></o:p></span></p><p class=MsoNormal><span style='font-size:11.0pt;font-family:"Calibri","sans-serif";color:#1F497D'><o:p> </o:p></span></p><p class=MsoNormal><span style='font-size:11.0pt;font-family:"Calibri","sans-serif";color:#1F497D'> Indeed, I reference your paper, though I don’t discuss it. But the main point to Hugh is that this type of heating (in the corona, transition region, or even upper chromosphere) won’t produce spicules.<o:p></o:p></span></p><p class=MsoNormal><span style='font-size:11.0pt;font-family:"Calibri","sans-serif";color:#1F497D'><o:p> </o:p></span></p><p class=MsoNormal><span style='font-size:11.0pt;font-family:"Calibri","sans-serif";color:#1F497D'>Cheers,<o:p></o:p></span></p><p class=MsoNormal><span style='font-size:11.0pt;font-family:"Calibri","sans-serif";color:#1F497D'>Jim<o:p></o:p></span></p><p class=MsoNormal><span style='font-size:11.0pt;font-family:"Calibri","sans-serif";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-bounces@solar.physics.montana.edu [mailto:loops-bounces@solar.physics.montana.edu] <b>On Behalf Of </b>Viggo Hansteen<br><b>Sent:</b> Tuesday, July 31, 2012 1:31 PM<br><b>To:</b> A mailing list for scientists involved in the observation and modeling of solar loop structures<br><b>Subject:</b> Re: [Loops] type II spicule paper<o:p></o:p></span></p></div></div><p class=MsoNormal><o:p> </o:p></p><p class=MsoNormal>No one has doubted that there is heating at great heights. Question is where the bulk of the nanoflares occur. As you know I think there are good reasons (the bulk of magnetic field does not rise high into the corona, except perhaps in coronal holes) to believe they occur in the vicinity of the transition region (including the upper chromosphere).<o:p></o:p></p><div><p class=MsoNormal>V.<o:p></o:p></p></div><div><p class=MsoNormal><o:p> </o:p></p><div><div><p class=MsoNormal>On Jul 31, 2012, at 17:14 , Klimchuk, James A. (GSFC-6710) wrote:<o:p></o:p></p></div><p class=MsoNormal><br><br><o:p></o:p></p><div><p class=MsoNormal><span style='font-size:11.0pt;font-family:"Calibri","sans-serif"'><br>Last point: why can't type-Ii spicules be the manifestation of nanoflares in a stratified inhomogeneous plasma?<o:p></o:p></span></p></div><div><p class=MsoNormal><span style='font-size:11.0pt;font-family:"Calibri","sans-serif";color:#1F497D'> </span><span style='font-size:11.0pt;font-family:"Calibri","sans-serif"'><o:p></o:p></span></p></div><div><p class=MsoNormal><span style='font-size:11.0pt;font-family:"Calibri","sans-serif";color:#1F497D'>Depends on where the nanoflares occur. Nanoflares that occur in the transition region or corona (in plasma that is originally hotter than 10^4 K) will not produce ejections of cold material. I have a discussion of this in the paper. Nanoflares that occur deep in the chromosphere, below the eventual spicule, can produce cold ejections.</span><span style='font-size:11.0pt;font-family:"Calibri","sans-serif"'><o:p></o:p></span></p></div><div><p class=MsoNormal><span style='font-size:11.0pt;font-family:"Calibri","sans-serif";color:#1F497D'> </span><span style='font-size:11.0pt;font-family:"Calibri","sans-serif"'><o:p></o:p></span></p></div></div><p class=MsoNormal><o:p> </o:p></p><div><div><div><p class=MsoNormal><span style='font-size:6.0pt;font-family:"Helvetica","sans-serif";color:black'>========================================================</span><span style='font-size:13.5pt;font-family:"Helvetica","sans-serif";color:black'><o:p></o:p></span></p></div><div><p class=MsoNormal><span style='font-size:6.0pt;font-family:"Helvetica","sans-serif";color:black'>Viggo H. Hansteen <a href="http://www.astro.uio.no/~viggoh">http://www.astro.uio.no/~viggoh</a></span><span style='font-size:13.5pt;font-family:"Helvetica","sans-serif";color:black'><o:p></o:p></span></p></div><div><p class=MsoNormal><span style='font-size:6.0pt;font-family:"Helvetica","sans-serif";color:black'>Institutt for teoretisk astrofysikk tel: +47-22856120</span><span style='font-size:13.5pt;font-family:"Helvetica","sans-serif";color:black'><o:p></o:p></span></p></div><div><p class=MsoNormal><span style='font-size:6.0pt;font-family:"Helvetica","sans-serif";color:black'>PB 1029, Blindern fax: +47-22856505</span><span style='font-size:13.5pt;font-family:"Helvetica","sans-serif";color:black'><o:p></o:p></span></p></div><div><p class=MsoNormal><span style='font-size:6.0pt;font-family:"Helvetica","sans-serif";color:black'>N-0315 Oslo, Norway <a href="mailto:Viggo.Hansteen@astro.uio.no">Viggo.Hansteen@astro.uio.no</a></span><span style='font-size:13.5pt;font-family:"Helvetica","sans-serif";color:black'><o:p></o:p></span></p></div><div><p class=MsoNormal><span style='font-size:6.0pt;font-family:"Helvetica","sans-serif";color:black'>========================================================</span><span style='font-size:13.5pt;font-family:"Helvetica","sans-serif";color:black'><o:p></o:p></span></p></div></div></div><p class=MsoNormal><o:p> </o:p></p></div></div></div></body></html>