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Messages 232 - 264 of 622   Oldest  |  < Older  |  Newer >  |  Newest
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232
Just a caution here. If the radio emission from a Cloudy PN model is optically thin then the code calculates it properly. However at high enough densities or...
kevin_m_volk
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Apr 17, 2007
1:57 am
233
Hi Kevin, This is a well known problem. The bottom line is that you can get the correct answer for optically thick conditions only by using exact radiative...
peter_van_hoof
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Apr 17, 2007
10:57 am
234
... Hi Kevin, just for the record, could you please upload the input script for a sim that shows this problem? thanks! Gary...
gary_ferland
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Apr 17, 2007
2:56 pm
235
Hi, I recently update to c07 and the way I was automaticaly reading the output files in Cloudy_3D doesn't work anymore. I realized that some of the formats...
chris_morisset
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Apr 25, 2007
9:52 pm
236
Hi Christophe all of the punch output is moving over to tab delimited fields. This makes it much easier to deal with the data from the command prompt, since...
gary_ferland
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Apr 26, 2007
1:54 am
237
Hi, Following with the surprises I meet since the upgrade to c07_02, I found that the Sulphur lines are changed by a big factor. [SII] is strongly decreased...
chris_morisset
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Apr 26, 2007
6:36 pm
238
Hi Gary, Thanks for the answer, I switch to reading in free format and it's working fine.Christophe...
chris_morisset
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Apr 26, 2007
6:42 pm
239
Hi Christophe actually Jan Simpson asked the same question a few days ago ... The S ions are from Badnell ApJ, 379, 356. They are listed down to log T = 4.5...
gary_ferland
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Apr 26, 2007
7:15 pm
240
Thanks Gary for the tip to print out the coeffs. The c07_2 Cloudy answer is: nelem=15 SULP, RR then DR -1.00e+00 -1.00e+00 -1.00e+00 -1.00e+00 5.52e-12...
chris_morisset
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Apr 26, 2007
8:16 pm
241
Hi, I am Haibo, Yuan from Peking University. In my model of the PN NGC 6153, the dielectronic recombination coefficients of S are assumed to be the...
yuanhb_pku
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Apr 27, 2007
3:52 am
242
Thanks a lot Yuan, I think that this is more one time a proof that ISM is sometimes the best way to determine atomic phuysics parameters.... Cheers, Christophe...
chris_morisset
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Apr 27, 2007
6:15 pm
243
There are still something not clear for me in the output of the RR and DR coefficients. From what I undestood, to compare between c06 and c07 (resp), one must ...
chris_morisset
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Apr 27, 2007
8:56 pm
244
Hi there, Here is what is going on. I would especially appreciate hearing what Christophe, Yuan, and Jan think. The plan is for all DR and RR data to...
gary_ferland
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Apr 28, 2007
3:37 pm
245
Hi Gary, Thanks a lot for this clear message about the DR coeffs and the difficulties we all meet using them! I think this is always a good idea to add options...
chris_morisset
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Apr 30, 2007
6:34 pm
246
Hi Gary and Christophe, Thanks for sharing your ideas. I am concerned about the effects on the model results caused by the uncertainties of the DR of...
yuanhb_pku
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May 2, 2007
5:42 am
247
Greetings, A release candidate for C07.02.01, a bugfix roll up of C07.02, is posted on the ftp site. It is available only as a large tarball under the...
gary_ferland
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May 4, 2007
4:34 pm
249
Hi Gary, Some years ago you helped me construct a diagnostic ratio of Brgamma to FIR (C90, FIR=total 40um to 250 um). I was analyzing an HII region in the...
rdblum5
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May 11, 2007
5:17 pm
250
... the continuum bands are controlled by the bands_continuum.dat file in the data directory. You could change the FIR definition back to the old value and...
gary_ferland
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May 11, 2007
8:42 pm
251
Hi Gary, Thanks. By version, I assume you mean c90 and c70.02. I will run a comparison. The difference shouldn't be in the bands because the newer band...
Bob Blum
rdblum5
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May 11, 2007
9:02 pm
252
Something major must be changing to cause what you see. Check the geometry. it is possible that the old models were plane parallel and the new ones are...
gary_ferland
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May 12, 2007
2:11 am
254
Hi, Does Cloudy include in calculation L-shell iron lines? There seems to be an iron line of this kind (around 1.61 keV) in my data and I can't model it with...
astronerma
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May 13, 2007
12:02 pm
255
... Hi Ania They should be there. What ionization stage is Fe? if low ionization then the lines are produced by fluorescence, if high charge then by ...
gary_ferland
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May 13, 2007
4:34 pm
256
Hi Gary, Thanks for quick reply, The line that best suits me is of highly ionized iron so as you say it should be produced by collisions, but what concerns me,...
astronerma
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May 13, 2007
7:43 pm
257
Dear Gary, I'm trying to reproduce some calculations I did years ago with Cloudy 96.01, using Cloudy 07.02.00. However, results are very different and I don't...
burkinafaso76
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May 18, 2007
11:19 am
258
Hi, Just scratched my head regarding some complaints from Cloudy (version 07.02.01) about my input SED being outside the allowed dynamical range. It seems that...
Jarle Brinchmann
jarlebrinchmann
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May 29, 2007
12:23 pm
260
... range. It ... happens is ... script does ... spectrum ... in the ... being ... normalisation ... with me. ... Hi Jarle, yes, there are obviously a few...
gary_ferland
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May 30, 2007
1:24 am
261
... Hi Stefano, this is mainly to let you know that I am looking into it, but at a low level for now. Next week will be better. The biggest single different...
gary_ferland
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May 30, 2007
2:52 pm
262
Are any of these warnings worth worrying about? ... mole_h2.cpp: In function void H2_collid_rates(): mole_h2.cpp:1641: warning: format %i expects type int, but...
Kirk Korista
qso_korista
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May 30, 2007
6:53 pm
263
Gary, Using 07.02.01, compiled with g++ under the optimized options, I ran a program which optimizes log U and log N for a fixed value of hden, but under...
Kirk Korista
qso_korista
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May 30, 2007
7:17 pm
264
Hi Gary, thanks for the reply, but the inclusion of those lines doesn't make such a big difference in my case. Results from the new version of cloudy still...
burkinafaso76
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May 31, 2007
10:31 am
Messages 232 - 264 of 622   Oldest  |  < Older  |  Newer >  |  Newest
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