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<TITLE>RE: [Loops] EIS AR Loops - Tripathi et al, 2009, ApJ</TITLE>
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<P><FONT SIZE=2>Dear Leon, dear all,<BR>
<BR>
I would like to mention that we also have MHD seismological evidence<BR>
of fine structuring of the hot corona, e.g.<BR>
<BR>
\bibitem[van Doorsselaere et<BR>
al.(2008)]{2008A&A...491L...9V} van Doorsselaere, T., Brady, C.~S., Verwichte, E., Nakariakov, V.~M.\ 2008.\ Seismological demonstration of perpendicular density structuring in the solar corona.\ Astronomy and Astrophysics 491, L9-L12.<BR>
<BR>
<A HREF="http://adsabs.harvard.edu/abs/2008A%26A...491L...9V">http://adsabs.harvard.edu/abs/2008A%26A...491L...9V</A> <BR>
<BR>
All the best,<BR>
<BR>
Valery<BR>
<BR>
<BR>
<BR>
-----Original Message-----<BR>
From: loops-bounces@mithra.physics.montana.edu on behalf of Leon Golub<BR>
Sent: Tue 06/01/2009 18:50<BR>
To: loops@mithra.physics.montana.edu<BR>
Cc: H.E.Mason@damtp.cam.ac.uk<BR>
Subject: Re: [Loops] EIS AR Loops - Tripathi et al, 2009, ApJ<BR>
<BR>
Helen et al.,<BR>
<BR>
I can't let this go uncommented. Even though this paper was<BR>
accepted (I know, I was the editor) I disagree with the conclusion<BR>
that hot loops are fuzzier. Yes, that's what you see, but it is<BR>
also explainable if the hot parts of the AR have many fine threads<BR>
(unresolved at present resolution) with a large filling factor.<BR>
That as the conclusion Joan and I came to from analyzing 284A<BR>
data.<BR>
<BR>
Anyway, this won't be settled until we fly an imager with higher<BR>
resolution. We're proposing one this year and I'm hoping we get<BR>
the chance to clear this up, finally.<BR>
Cheers,<BR>
<BR>
Leon<BR>
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