Helen et al,

Congratulations to the new dazzling Hinode paper!

On the same note, from the statistics of some 18,000 loop widths 
measurements in the 3 TRACE filters we found a slight dependence 
that loops become wider (or fuzzier) with temperatures, i.e.,

w(T) ~ T^(1.3+/-0.7)

(see Aschwanden, Nightingale, & Boerner 2007, ApJ 656, 577).
So loops at T=2 MK are about a factor of 3 fatter than at T=1 MK.
The inferred coronal filling factors vary also slightly with temperature,
from q~0.74 at T=1 MK to q~0.32 at T=2 MK, which goes along the
lines Leon suggests.

Cheers,
Markus


On Jan 6, 2009, at 1:08 PM, reale@astropa.unipa.it wrote:

I agree with Leon, but I also think that the paper only certifies that the
loops look fuzzier in hotter lines. There may be no real contradiction
with Leon's perspective. Of course, we all sustain Leon's new imager.
Ciao
Fabio

Helen et al.,

I can't let this go uncommented. Even though this paper was
accepted (I know, I was the editor) I disagree with the conclusion
that hot loops are fuzzier. Yes, that's what you see, but it is
also explainable if the hot parts of the AR have many fine threads
(unresolved at present resolution) with a large filling factor.
That as the conclusion Joan and I came to from analyzing 284A
data.

Anyway, this won't be settled until we fly an imager with higher
resolution. We're proposing one this year and I'm hoping we get
the chance to clear this up, finally.
Cheers,

Leon
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____________________________________________
Dr. Markus J. Aschwanden
Solar & Astrophysics Laboratory
Lockheed Martin Advanced Techology Center
Org. ADBS, Bldg. 252
3251 Hanover St., Palo Alto, CA 94304, USA
Phone: 650-424-4001, FAX: 650-424-3994
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