Dear Leon, dear all,
I would like to mention that we also have MHD seismological evidence of fine structuring of the hot corona, e.g.
\bibitem[van Doorsselaere et 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.
http://adsabs.harvard.edu/abs/2008A%26A...491L...9V
All the best,
Valery
-----Original Message----- From: loops-bounces@mithra.physics.montana.edu on behalf of Leon Golub Sent: Tue 06/01/2009 18:50 To: loops@mithra.physics.montana.edu Cc: H.E.Mason@damtp.cam.ac.uk Subject: Re: [Loops] EIS AR Loops - Tripathi et al, 2009, ApJ
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 _______________________________________________ Loops mailing list Loops@solar.physics.montana.edu https://mithra.physics.montana.edu/mailman/listinfo/loops