<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 4.01 Transitional//EN">
<html>
<head>
<meta content="text/html; charset=ISO-8859-1"
http-equiv="Content-Type">
</head>
<body bgcolor="#ffffff" text="#000000">
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">
<meta http-equiv="content-type" content="text/html;
charset=ISO-8859-1">
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>
<pre wrap="">
<fieldset class="mimeAttachmentHeader"></fieldset>
_______________________________________________
Loops mailing list
<a class="moz-txt-link-abbreviated" href="mailto:Loops@solar.physics.montana.edu">Loops@solar.physics.montana.edu</a>
<a class="moz-txt-link-freetext" href="https://mithra.physics.montana.edu/mailman/listinfo/loops">https://mithra.physics.montana.edu/mailman/listinfo/loops</a>
</pre>
</blockquote>
<br>
<pre class="moz-signature" cols="72">--
______________________________________________________________________
Alan GABRIEL <a 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
_____________________________________________________________________
</pre>
</body>
</html>