There are several versions of the atom files used to build the comp-type atoms.

if just e.g. atom_fe13-- it is what Phil Judge gave me in 2024 (and which appear to have been created in DIPER in 2020). 
(note the old files FORWARD used to use live in PHIL_OLD_2006)

For three ions, fe13, si10, and si9 -- I have updates from Alin Parashiv (e.g. alin_atom_fe13) which appear to have been written in 2020 at the same time as the ones Phil sent me -- and include "** Line to account for Sascha's calculation." and also appear to have maximum wavelenght (in units of QNORM) of 10 instead of 30

For these same three ions, I have updated the abundances to the most recent Chromospheric and photospheric abundances, to be consistent with the latest in FORWARD (otherwise, Phil's code outputs a very old version of chianti abundances). These are identified with the prefixes C_ and P_.  ***The default in FORWARD is to use the abundance-updated versions for these three atoms***

Note that FORWARD has had fe11,fe13,fe14,si9, and si10 for a while.

FE10 was added more recently. And then at the same time I requested some non Iron lines for comparison to UCoMP, AR13, S9, S11. Notes on these updates can be found in the emails from Phil below.

**Note that I have *not* checked/updated abundances for fe10, fe11, fe14, ar13, s9, s11, and FORWARD defaults to the versions sent to me by Phil in 2024 .**

Finally, Phil creates "input" files (which are in the directory PHIL_INPUT_FILES) -- this information is incorporated within the FORWARD code, for_compdefaults.pro in the DEFAULTS directory.





Below are emails from Phil
---------------------

Here is also S IX included along with all available atoms and input files now.

S IX is not easy to model to get intensities and polarization correct with a 
smaller atom and my fudge factor approach.

I will probably not build something for S XIII later because this is 
Be- like (I missed the "e" in my earlier email), the M1 transitions lie between 
the 3P states some 250 eV above the ground 1S state.  It's  in the triplet system
like He 10830 but while 10830 is E1 transitions,   these are transitions between the 
2s 2p 3PO metastable levels. Only the J=0, 2 levels are metastable of this excited term.
The J=1 level decays fast to the ground level via relativistic effects so
it will have a small population.   S XIII will therefore have almost no polarization 
because it will be populated only by collisions.   It is going to be dim, about 0.001 of the resonance
line at 256.68 Angstrom. 

so I think my job is done.


On Mon, Feb 26, 2024 at 6:04 PM Sarah Gibson <sgibson@ucar.edu> wrote:
Thanks, Phil!

On Mon, Feb 26, 2024 at 5:23 PM Philip Judge <judge@ucar.edu> wrote:

Here are atomic/input  models for Ar XIII.  Formed near 10^6.4 K, there is little 
contribution from cascades from the higher levels, nor any need for 
cecoeff > 0.

Also for isolectronic S XI, where I added some depolarizing transitions to mimic
depolarization from E1 lines.  

The files appended with "big" are large multi-level atoms including the strongest E1
transitions which decay to the upper levels of the smaller atoms, and should include 
all depolarization rates and collisional excitations needed,   I matched output of
one with the other to make the smaller files.    For the runs use the not big files





On Thu, Feb 22, 2024 at 5:16 PM Philip Judge <judge@ucar.edu> wrote:

Fe X attached, it will take a little while to build the other non-Fe ions, 
one morning should be enough, I have to add in special energy level to mimic
collisions from tens of real levels.

On Thu, Feb 22, 2024 at 1:39 PM Sarah Gibson <sgibson@ucar.edu> wrote:
Thanks, Phil! This is helpful.

In addition to the Fe13 and Si10 bold-faced below, FORWARD currently has Fe11, Fe14, and Si9. So I think the only one missing from your current list is Fe10. Could you send me your CLE files (atom, input) for Fe10?

And then, any other lines you build I'd be happy to add.

cheers
Sarah


On Thu, Feb 22, 2024 at 10:51 AM Philip Judge <judge@ucar.edu> wrote:


Here are the atomic ions for which I have built suitable small numbers of
levels to make them tractable for production work with cle.

atom.fe10 (i.e. Fe X)
atom.fe11
atom.fe13
atom.fe14
 atom.si10
 atom.si9

so nothing so far but Fe and Si.   

Ar XIII is isoelectronic with C and so 
will have a ^3P_{0,1,2} ground level structure (like Fe XIII).  

S XIII is isoelectronic with B and so has a ^1S_0 ground state.
The transition at 1083 nm will be between metastable ^3P levels at 24 eV
(in this sense it is a bit like He I 1083 but with n=2 instead of n=1)

S XI is isoelectronic with C just like Ar XIII
S IX is isoelectronic with O so has ^3P_{2.1.0} like Fe XI with J=2 lowest level
(Hund's rule).  

I would expect the S XIII line to be relatively weak based on the 
isoelectronic line of Si XI at 1933 nm computed in my 1998 paper

I'll build suitable models for the other ions including the usual 
equivalent level to include cascades from levels excited by E1 
transitions








On Wed, Feb 21, 2024 at 8:50 AM Sarah Gibson <sgibson@ucar.edu> wrote:
Hi Phil -- I heard from Jenna Samra that these are the lines she'll be observing for the eclipse. I'm wondering if you know which of these could be modeled in CLE? The bold-faced are the ones already in FORWARD, but if the others are possible and you could provide atom and input files I could add them.

Also cc'ing Roberto and  Momo since they are working with Hanle RT including 10830.

Jenna is on an ISSI team that I am also on (also Supriya who gave the colloquium a week or so ago). Our intention is to set up some benchmark solar corona to forward model and compare results.

===lines in the ACES passband:

1014nm Ar XIII
1030nm S XIII
1075nm Fe XIII
1080nm Fe XIII
1083nm He I
1252nm S IX
1393nm S XI
1430nm Si X

cheers
Sarah
--
