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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Loops(a)solar.physics.montana.edu
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Hi Loopsters,
We enjoyed a very successful workshop in Mallorca. Many thanks to the SOC and LOC and especially to their chairs, Inaki Ugarte Urra and Jose Luis Ballester, respectively. These guys put in a lot of hard work.
We also thank Spiro Antiochos, Joan Schmelz, and Robert Walsh, whose terms on the Steering Committee are ending. Please send me nominations for their replacements, including self nominations. The Steering Committee will then vote from a list of candidates. (Spiro, Joan, and Robert are eligible to serve again.)
It's never too early to start planning for the next workshop, in 2 years. Please contact me if you are interested in hosting. We have some tentative offers already, but they are highly tentative at this time.
Best wishes,
Jim
********************************************************************************
James A. Klimchuk
NASA Goddard Space Flight Center
Solar Physics Lab, Code 671
Bldg. 21, Rm. 158
Greenbelt, MD 20771
USA
Phone: 1-301-286-9060
Fax: 1-301-286-7194
E-mail: James.A.Klimchuk(a)nasa.gov<mailto:James.A.Klimchuk@nasa.gov>
Home page: http://science.gsfc.nasa.gov/671/staff/bios/cs/James_Klimchuk_ssi.html
No endorsement by NASA is implied for any correspondence related to my role as an officer of professional organizations (American Geophysical Union, American Astronomical Society, International Astronomical Union).
********************************************************************************
Dear colleagues
please find at the following link the preprint of a work accepted
for publication in ApJ, showing interesting evidence of thermal
instability in UV light curves late in a flare. This analysis is done on
SoHO/SUMER data but may be useful for flare observations with SDO/EVE:
http://arxiv.org/abs/1111.3579
The abstract is below.
Best regards
Fabio Reale
Post-flare UV light curves explained with thermal instability of loop plasma
F. Reale, E. Landi, S. Orlando
In the present work we study the C8 flare occurred on September 26, 2000
at 19:49 UT and observed by the SOHO/SUMER spectrometer from the
beginning of the impulsive phase to well beyond the disappearance in the
X-rays. The emission first decayed progressively through equilibrium
states until the plasma reached 2-3 MK. Then, a series of cooler lines,
i.e. Ca x, Ca vii, Ne vi, O iv and Si iii (formed in the temperature
range log T = 4.3 - 6.3 under equilibrium conditions), are emitted at
the same time and all evolve in a similar way. Here we show that the
simultaneous emission of lines with such a different formation
temperature is due to thermal instability occurring in the flaring
plasma as soon as it has cooled below ~ 2 MK. We can qualitatively
reproduce the relative start time of the light curves of each line in
the correct order with a simple (and standard) model of a single flaring
loop. The agreement with the observed light curves is greatly improved,
and a slower evolution of the line emission is predicted, if we assume
that the model loop consists of an ensemble of subloops or strands
heated at slightly different times. Our analysis can be useful for flare
observations with SDO/EVE.