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Thank you very much, Alan. I totally agree. I also look forward to
having broadband high-resolution X-ray spectroscopy of the non-flaring
corona not too far in the future! <br>
Fabio<br>
<br>
On 06/09/2011 01:56 PM, Alan Gabriel wrote:
<blockquote cite="mid:4DF0B4E2.2060307@ias.u-psud.fr" type="cite">
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A nice paper and an important contribution to the debate. But the jury
is still out. We may never resolve this without real spectroscopic
evidence of the very hot component. Where is our future spectroscopy
coming from??<br>
<br>
Alan Gabriel<br>
<br>
<br>
Le 09/06/2011 10:52, Fabio Reale a écrit :
<blockquote cite="mid:4DF089B4.3060109@astropa.unipa.it" type="cite">
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Dear colleagues<br>
please find at the following link the preprint of a work accepted
for publication on the ApJ Letters, showing new strong evidence of
finely-structured loops with impulsive nanoflare activity in active
regions:<br>
<br>
<a moz-do-not-send="true" class="moz-txt-link-freetext"
href="http://arxiv.org/abs/1106.1591">http://arxiv.org/abs/1106.1591</a><br>
<br>
The abstract is below.<br>
<br>
Best regards<br>
Fabio Reale<br>
<br>
<h1 class="title"><small><small><small>Solar Dynamics Observatory
discovers thin high temperature strands in coronal active regions</small></small></small></h1>
<div class="authors"><span class="descriptor">Authors:</span> Fabio
Reale, Massimiliano Guarrasi, Paola Testa, Edward E. DeLuca, Giovanni<br>
Peres, Leon Golub<br>
<br>
</div>
<blockquote class="abstract"> <span class="descriptor">Abstract:</span>
One scenario proposed to explain the million degrees solar corona is a
finely-stranded corona where each strand is heated by a rapid pulse.
However, such fine structure has neither been resolved through direct
imaging observations nor conclusively shown through indirect
observations of extended superhot plasma. Recently it has been shown
that the observed difference in appearance of cool and warm coronal
loops (~1 MK, ~2-3 MK, respectively) -- warm loops appearing "fuzzier"
than cool loops -- can be explained by models of loops composed of
subarcsecond strands, which are impulsively heated up to ~10 MK. That
work predicts that images of hot coronal loops (>~6 MK) should again
show fine structure. Here we show that the predicted effect is indeed
widely observed in an active region with the Solar Dynamics
Observatory, thus supporting a scenario where impulsive heating of fine
loop strands plays an important role in powering the active corona. </blockquote>
<br>
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<br>
<pre class="moz-signature" cols="72">--
______________________________________________________________________
Alan GABRIEL <a moz-do-not-send="true"
class="moz-txt-link-abbreviated"
href="mailto:alan.gabriel@ias.u-psud.fr">alan.gabriel@ias.u-psud.fr</a>
Institut d'Astrophysique Spatiale tel : (33) 1 69 85 85 10
Batiment 121, Universite Paris XI fax : (33) 1 69 85 86 75
91405 ORSAY Cedex mobile : (33) 6 72 14 23 89
France
_____________________________________________________________________
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