Hi everyone,
In the spirit of a number of recent papers that have been focused on trying
to determine the dominant components of the emission in the wavelength
channels of imaging instruments (AIA, in particular), Jim and I would like
to share with you all a link to a paper on this very topic that was recently
published in the ApJ Supplement Series:
http://iopscience.iop.org/0067-0049/194/2/26/pdf/apjs_194_2_26.pdf
Our aim in carrying out the work described in this paper was to provide a
large amount of quantitative data from our modeling studies that we hope
will be of use in the analysis of observationally gathered data.
Best wishes,
Steve
-----Original Message-----
From: loops-bounces(a)solar.physics.montana.edu
[mailto:loops-bounces@solar.physics.montana.edu] On Behalf Of Paola Testa
Sent: Tuesday, September 20, 2011 10:00 AM
To: A mailing list for scientists involved in the observation and modeling
of solar loop structures
Cc: Juan Martinez Sykora
Subject: [Loops] Forward modeling of emission in SDO/AIA passbands from
dynamic 3D simulations
Hello all,
here is a link to a preprint of a paper, accepted for publication on ApJ,
that is also discussing issues related to the interpretation of AIA
observations:
http://adsabs.harvard.edu/abs/2011arXiv1109.0704M
cheers,
Paola
On 9/9/11 12:03 PM, Giulio Del Zanna wrote:
>
> Dear colleagues,
>
> here is a link to a preprint that discusses various
> (important) issues related to the interpretation of AIA data:
>
> http://solar.physics.montana.edu/cgi-bin/eprint/index.pl?entry=15555
>
> Those of you that were present at the excellent Mallorca meeting might
> recall the issues we raised there. The paper, which follows on from
> O'Dwyer et al., contains more.
>
> I encourage all to follow the example in the Appendix to calculate
> your own AIA responses using CHIANTI. We will soon release v.7, but do
> not expect huge differences.
> We are working to try and improve the atomic data for AIA, more to come.
>
>
> best wishes,
_______________________________________________
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Dear All,
We were informed that "your manuscript, "Prominence-cavity regions
observed using SWAP 174A filtergrams and simultaneous eclipse flash
spectra", by Bazin, C. Koutchmy, S. and Tavabi, E. has been accepted for
publication in Solar Physics."
A preprint is available at:
http://arxiv.org/abs/1207.1857
Note it is the 1st time that prominences and the so-called cavity often
seen above eclipse prominences are analyzed using a high spectral
resolution near the HeI and the HeII lines simultaneously with high S/N
ratio SWAP filtergrams at 174A and with EIT filtergrams, shedding some
light on the prominence-corona interacting region physics.
Please find after an abstract of the paper.
Feel free to contact the authors in case some additional material is
needed.
Enjoy!
Best,
Serge
-------------------------------------------------------------
At the occasion of the last solar total eclipse of 11th July, 2010, we
studied SWAP filtergrams (from the PROBA2 mission) taken at 17.4 nm in
the Fe IX/X lines with simultaneous slitless flash spectra in the
spectral region of 470 nm. These eclipse flash spectra showed many faint
low excitation emission lines with He I 471.3 nm and He II 468.6 nm
Paschen {\alpha} chromospheric lines, and correspond to off-limb
prominences regions observed with space-borne imagers. We aligned and
stacked 80 individual spectra to study some modulations intensities
along the continuum between the monochromatic images of the prominences
without parasitic scattered light. We observed intensity depressions
around the continuum between prominences in both eclipse and SWAP
images. The prominence cavities are associated with a depression of the
plasma density, produced in the interface regions between the corona and
the prominences. Photometric measurements are shown at different scales
and different narrow spectral intervals, for both the prominences and
the coronal background.
Comments: 20 pages, 15 figures.
Dear all,
Just wanted to let you know about our new paper just published in the
Astrophysical Journal.
Is Active Region Core Variability age dependent?
Ignacio Ugarte-Urra and Harry P. Warren
The presence of both steady and transient loops in active region cores
has been reported from soft X-ray and extreme-ultraviolet observations
of the solar corona. The relationship between the different loop
populations, however, remains an open question. We present an
investigation of the short-term variability of loops in the core of two
active regions in the context of their long-term evolution. We take
advantage of the nearly full Sun observations of /STEREO/ and /Solar
Dynamics Observatory/ spacecraft to track these active regions as they
rotate around the Sun multiple times. We then diagnose the variability
of the active region cores at several instances of their lifetime using
EIS//Hinode/ spectral capabilities. We inspect a broad range of
temperatures, including for the first time spatially and temporally
resolved images of Ca XIV and Ca XV lines. We find that the active
region cores become fainter and steadier with time. The significant
emission measure at high temperatures that is not correlated with a
comparable increase at low temperatures suggests that high-frequency
heating is viable. The presence, however, during the early stages, of an
enhanced emission measure in the "hot" (3.0-4.5 MK) and "cool" (0.6-0.9
MK) components suggests that low-frequency heating also plays a
significant role. Our results explain why there have been recent studies
supporting both heating scenarios.
http://iopscience.iop.org/0004-637X/761/1/21/
Best regards,
Ignacio
--
~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~ ~
~ Ignacio Ugarte-Urra ~
Naval Research Laboratory. Code 7681.
4555 Overlook Ave SW. Washington, DC 20375
phone: (+1) 202 404 1779
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