<html><head><meta http-equiv="Content-Type" content="text/html charset=windows-1252"></head><body style="word-wrap: break-word; -webkit-nbsp-mode: space; -webkit-line-break: after-white-space;">That’s how it appears to me too. I’d add that the localization of the free energy is a difficult subject, and it may be misleading just to identify it with the B^2/8pi excess. This is because the realization of the free energy, i.e. its actual definition, depends on the nature of the instability that releases it. Understanding this requires understanding the boundary conditions, so it must be a higher-order theoretical matter.<div><br></div><div>Hugh</div><div><br><div><div>On Apr 14, 2015, at 8:42 AM, Serge Koutchmy <<a href="mailto:koutchmy@iap.fr">koutchmy@iap.fr</a>> wrote:</div><br class="Apple-interchange-newline"><blockquote type="cite">
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<div class="moz-cite-prefix">Thank you Markus for the preprint. <br>
Looking at your most important Fig. 3, you give the impression
that MORE free energy is available in the corona AFTER the peak of
the flare (GOES HXR, SXR emissions, etc) than before. <br>
Is not exactly the opposite of what we would wait following your
Introductory presentation of the topic and even the title of the
paper? <br>
Or did I miss something fundamental? <br>
Best, <br>
S. <br>
<br>
Le 13/04/2015 21:06, Markus J. Aschwanden a écrit :<br>
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<span style="font-family: Times; font-size: inherit;"> Aschwanden,M.J.
. 2015, ApJL ... (revised, 2015 Apr 2)</span><br style="font-family: Times;">
<a moz-do-not-send="true" href="http://www.lmsal.com/%7Easchwand/eprints/2015_iris.pdf" style="font-family: Times;">URL1="http://www.lmsal.com/~aschwand/eprints/2015_iris.pdf"</a><span style="font-family: Times; font-size: inherit;"> </span><br style="font-family: Times;">
<span style="font-family: Times; font-size: inherit;"></span><font style="font-family: Times;" size="4">Magnetic energy dissipation
during the 2014 Mar 29 flare: </font>
<div><font style="font-family: Times;" size="4">Consistent
measurements in the transition region and corona with IRIS and
AIA/SDO</font>
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<div style="word-wrap: break-word; -webkit-nbsp-mode: space;
-webkit-line-break: after-white-space; ">Dr. Markus J.
Aschwanden<br>
Solar & Astrophysics Laboratory<br>
Lockheed Martin Advanced Techology Center<br>
A021S, Bldg. 252<br>
3251 Hanover St., Palo Alto, CA 94304, USA<br>
Phone: 650-424-4001, FAX: 650-424-3994<br>
URL: <a moz-do-not-send="true" href="http://www.lmsal.com/%7Easchwand/">http://www.lmsal.com/~aschwand/</a><br>
e-mail: <a moz-do-not-send="true" href="mailto:aschwanden@lmsal.com">aschwanden@lmsal.com</a><br>
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