<html><head></head><body bgcolor="#FFFFFF"><div>Hi Jim, </div><div><br></div><div>Just scanned through, will send you comments after a thorough reading, but looks like a fair discussion. Couple of points though:</div><div><br></div><div>Are "A" waves a viable energetic supply to the corona? They get no mention and I understand that the net effect of their dissipation would be nanoflares-like heating distribution. </div><div><br></div><div>Btw, in addition to the above, discriminatory studies of quiet and coronal hole plasmas hold the key to the down-up (evaporative) vs up-down (type 2 "initiated") mass components of the mass cycle. It is a real push to expect the original energy supply for them to be different, but in one the coronal backwash is missing. The (detailed) study of the multi-component line profiles between the two should show the relative weighting of evaporative processes (regardless of their origin - see above) in the QS. My student has done a pretty detailed study of this and is about to submit a paper on her results - I will distribute to the list once submitted.</div><div><br></div><div>Last point: why can't type-Ii spicules be the manifestation of nanoflares in a stratified inhomogeneous plasma?</div><div><br>Cheers, Scott<div><br></div><div>Sent from my iPhone</div><div><br></div><div>Dr. Scott W. McIntosh</div><div>High Altitude Observatory</div><div>NCAR/UCAR, Boulder CO<span class="Apple-style-span" style="-webkit-tap-highlight-color: rgba(26, 26, 26, 0.296875); -webkit-composition-fill-color: rgba(175, 192, 227, 0.230469); -webkit-composition-frame-color: rgba(77, 128, 180, 0.230469); "> </span></div><div><span class="Apple-style-span" style="-webkit-tap-highlight-color: rgba(26, 26, 26, 0.296875); -webkit-composition-fill-color: rgba(175, 192, 227, 0.230469); -webkit-composition-frame-color: rgba(77, 128, 180, 0.230469); ">off: (303) 497-1544</span></div><span class="Apple-style-span" style="-webkit-tap-highlight-color: rgba(26, 26, 26, 0.292969); -webkit-composition-fill-color: rgba(175, 192, 227, 0.230469); -webkit-composition-frame-color: rgba(77, 128, 180, 0.230469);">mob: (720) 340-6263</span></div><div><br>On Jul 31, 2012, at 7:47, "Klimchuk, James A. (GSFC-6710)" <<a href="mailto:james.a.klimchuk@nasa.gov">james.a.klimchuk@nasa.gov</a>> wrote:<br><br></div><div></div><blockquote type="cite"><div><meta http-equiv="Content-Type" content="text/html; charset=us-ascii"><meta name="Generator" content="Microsoft Word 12 (filtered medium)"><style><!--
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</o:shapelayout></xml><![endif]--><div class="WordSection1"><p class="MsoNormal">Dear friends,<o:p></o:p></p><p class="MsoNormal"><o:p> </o:p></p><p class="MsoNormal"> You might be interested in my recent paper on “The Role of Type II Spicules in the Upper Solar Atmosphere,” which can be downloaded at <a href="http://arxiv.org/abs/1207.7048">http://arxiv.org/abs/1207.7048</a><o:p></o:p></p><p class="MsoNormal"><o:p> </o:p></p><p class="MsoNormal">Cheers,<o:p></o:p></p><p class="MsoNormal">Jim<o:p></o:p></p><p class="MsoNormal"><o:p> </o:p></p><p class="MsoNormal">ABSTRACT:<o:p></o:p></p><p class="MsoNormal">We examine the suggestion that most of the hot plasma in the Sun's <o:p></o:p></p><p class="MsoNormal">corona comes from type II spicule material that is heated as it is<o:p></o:p></p><p class="MsoNormal">ejected from the chromosphere. This contrasts with the traditional<o:p></o:p></p><p class="MsoNormal">view that the corona is filled via chromospheric evaporation that<o:p></o:p></p><p class="MsoNormal">results from coronal heating. We explore the observational<o:p></o:p></p><p class="MsoNormal">consequences of a hypothetical spicule dominated corona and conclude<o:p></o:p></p><p class="MsoNormal">from the large discrepancy between predicted and actual observations<o:p></o:p></p><p class="MsoNormal">that only a small fraction of the hot plasma can be supplied by<o:p></o:p></p><p class="MsoNormal">spicules (<2% in active regions and <5% in the quiet Sun). The<o:p></o:p></p><p class="MsoNormal">red-blue asymmetries of EUV spectral lines and the ratio of lower<o:p></o:p></p><p class="MsoNormal">transition region (LTR; T<0.1 MK) to coronal emission measures<o:p></o:p></p><p class="MsoNormal">are both predicted to be 2 orders of magnitude larger than observed. <o:p></o:p></p><p class="MsoNormal">Furthermore, hot spicule material would cool dramatically by<o:p></o:p></p><p class="MsoNormal">adiabatic expansion as it rises into the corona, so coronal heating<o:p></o:p></p><p class="MsoNormal">would be required to maintain the high temperatures that are seen at<o:p></o:p></p><p class="MsoNormal">all altitudes. The necessity of coronal heating is inescapable. <o:p></o:p></p><p class="MsoNormal">Traditional coronal heating models predict far too little emission<o:p></o:p></p><p class="MsoNormal">from the LTR, and we suggest that this emission comes primarily from<o:p></o:p></p><p class="MsoNormal">the bulk of the spicule material that is heated to <0.1 MK and<o:p></o:p></p><p class="MsoNormal">is visible in He II (304 A) as it falls back to the surface.<o:p></o:p></p><p class="MsoNormal"><o:p> </o:p></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">********************************************************************************</span><o:p></o:p></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">James A. Klimchuk</span><o:p></o:p></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">NASA Goddard Space Flight Center</span><o:p></o:p></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">Solar Physics Lab, Code 671</span><o:p></o:p></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">Bldg. 21, Rm. 158</span><o:p></o:p></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">Greenbelt, MD 20771</span><o:p></o:p></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">USA</span><o:p></o:p></p><p class="MsoNormal"> <o:p></o:p></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">Phone: 1-301-286-9060</span><o:p></o:p></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">Fax: 1-301-286-7194</span><o:p></o:p></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">E-mail: <a href="mailto:James.A.Klimchuk@nasa.gov"><span style="color:blue">James.A.Klimchuk@nasa.gov</span></a> </span><o:p></o:p></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">Homepage: </span><a href="https://sedupdate.gsfc.nasa.gov/sed/index.cfm?fuseAction=people.jumpBio&&iPhonebookId=15844">https://sedupdate.gsfc.nasa.gov/sed/index.cfm?fuseAction=people.jumpBio&&iPhonebookId=15844</a><o:p></o:p></p><p class="MsoNormal"> <o:p></o:p></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">No endorsement by NASA is implied for any correspondence related to my role as an officer of professional organizations (American Geophysical Union, International Astronomical Union, American Astronomical Society).<o:p></o:p></span></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif""> <o:p></o:p></span></p><p class="MsoNormal"><span style="font-size:10.0pt;font-family:"Arial","sans-serif"">********************************************************************************<o:p></o:p></span></p><p class="MsoNormal"> <o:p></o:p></p><p class="MsoNormal"><o:p> </o:p></p></div></div></blockquote><blockquote type="cite"><div><span>_______________________________________________</span><br><span>Loops mailing list</span><br><span><a href="mailto:Loops@solar.physics.montana.edu">Loops@solar.physics.montana.edu</a></span><br><span><a href="https://mithra.physics.montana.edu/mailman/listinfo/loops">https://mithra.physics.montana.edu/mailman/listinfo/loops</a></span><br></div></blockquote></body></html>