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<p><font size="+1">Dear Friends, <br>
</font></p>
<p><font size="+1">Please find in the link a paper on Fan loops
that is just published in ApJ. <br>
</font></p>
<p><font size="+1"><b><a class="moz-txt-link-freetext" href="http://iopscience.iop.org/article/10.3847/1538-4357/835/2/244/pdf">http://iopscience.iop.org/article/10.3847/1538-4357/835/2/244/pdf</a></b><br>
</font></p>
<p><font size="+1">Please let us know of any comments/suggestions
you have on the paper.</font></p>
<p><font size="+1">For your information, I copied the abstract
below:</font></p>
<p><font size="+1">Abstract: </font>A comprehensive study of the
physical parameters of active region fan loops is <br>
presented using the observations
recorded with the Interface Region Imaging Spectrometer <br>
(IRIS), the EUV Imaging Spectrometer (EIS) on board
Hinode, and the Atmospheric Imaging <br>
Assembly (AIA) and the Helioseismic and Magnetic Imager (HMI) on
board the Solar Dynamics <br>
Observatory (SDO). The fan loops emerging from non-flaring AR
11899 (near the disk
center) <br>
on 2013 November 19 are clearly discernible in AIA 171 Å images
and in those obtained in <br>
Fe VIII and
Si VII images using EIS. Our measurements of electron densities
reveal that the <br>
footpoints of these loops are at an
approximately constant pressure with electron densities <br>
of log Ne = 10.11 cm−3 at log [T/K ] T K = 5.15 (O IV), and
log Ne = 8.9 cm−3 at <br>
log [T/K] = 6.15 (Si X). The electron temperature diagnosed
across the fan loops by means
<br>
of EM-Loci suggest that two temperature components exist at log
[T/K ] = 4.95 at the footpoints. <br>
These
components are picked up by IRIS lines and EIS lines,
respectively. At higher heights, the loops <br>
are nearly
isothermal at log [T/K ] = 5.95, which remained constant along
the loop. The measurement <br>
of the Doppler shift
using IRIS lines suggests that the plasma at the footpoints of
these loops is <br>
predominantly redshifted by 2–3 km s−1
in C II, 10–15 km s−1 in Si IV, and 15–20 km s−1 in O IV, <br>
reflecting the increase in the speed of downflows with
increasing temperature from log [T/K ] = 4.40 to 5.15. <br>
These observations can be explained by low-frequency
nanoflares or impulsive heating, and provide <br>
further important constraints on the modeling of the dynamics of
fan
loops<font size="+1">.</font></p>
<p><font size="+1">Best,<br>
-Durgesh</font></p>
<p><font size="+1"><br>
</font></p>
<p><font size="+1"><br>
</font></p>
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