... | ... | @@ -14,7 +14,7 @@ source code documentation for C13 is available |
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Released 2017 Jan 24 at revision r11558. This is the final release from this branch and includes the following:
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*Support has been added for the Oracle Developer Studio compiler version 12.5.* For this compiler you need to compile in the *_sys_oraclestudio*_ subdirectory. See also important remarks regarding potential problems when using this compiler on the [wiki:CompilingCloudyC13] page.
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*Support has been added for the Oracle Developer Studio compiler version 12.5.* For this compiler you need to compile in the *sys_oraclestudio* subdirectory. See also important remarks regarding potential problems when using this compiler on the [wiki:CompilingCloudyC13] page.
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*Fixed several problems when running under FreeBSD 11.0-RELEASE.*
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... | ... | @@ -42,7 +42,7 @@ We fixed a bug where Cloudy would not compile when using the *Intel MPI implemen |
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We fixed a bug where Cloudy would not compile with *very recent versions of the g++ standard template library*.
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An internal floor on level populations generated *artificially strong metallic line emission*_ at very low densities, now fixed. Reported by Orly Gnat.
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An internal floor on level populations generated *artificially strong metallic line emission* at very low densities, now fixed. Reported by Orly Gnat.
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A bug when *optimizing emergent line ratios* has been fixed. The flux ratio was wrong because the intrinsic flux for the normalizing line was used rather than the emergent flux. The syntax for the command has also been clarified in Hazy. Reported by Jim Smith.
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... | ... | @@ -73,7 +73,7 @@ Changes to the makefile to *accommodates recent changes in OS X and its compiler |
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[Shaw+05](http://cdsads.u-strasbg.fr/abs/2005ApJ...624..794S) describes our implementation of the H,,2,, molecule, and the use of a ``g-bar`` approximation
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when no collision data are available.
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This approximation was not enabled by default for H,,2,, - H,,2,, collisions in C10 and C13.
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*_The g-bar approximation has been enabled*_. This raises the populations of high J levels for warm gas.
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*The g-bar approximation has been enabled*. This raises the populations of high J levels for warm gas.
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Thanks for Miguel Pereira Santaella for reporting this.
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*Print more helpful comment* when code stops with error
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... | ... | @@ -81,10 +81,10 @@ _PROBLEM ConvBase sets lgAbort since nPres2Ioniz exceeds limPres2Ioniz._ |
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The remedy is often to _Reset this limit with the SET PRES IONIZ command_.
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If the density decreases as radius increases there are a family of sims where the ionization will increase with radius, which will become quite large,
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as described in Hazy 1, Sec 8.8.2, "Clouds extending to infinity". *_We fixed an fpe*_ that could occur when this happens.
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as described in Hazy 1, Sec 8.8.2, "Clouds extending to infinity". *We fixed an fpe* that could occur when this happens.
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(You should specify an outer radius for such models.)
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Hazy 1 now explains that *_you cannot edit the SED file produced with the save transmitted continuum command*_.
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Hazy 1 now explains that *you cannot edit the SED file produced with the save transmitted continuum command*.
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Numerous small changes to Hazy 1.
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... | ... | @@ -116,7 +116,7 @@ Fixed by placing a cap on the minimum temperature used in evaluating that rate. |
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The *set C12C13 command*, and the default C12/C13 ratio, *only worked on the first sim in grids*. It was -1 in second and later sims in a grid.
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Under extreme conditions the *SAVE FITS* command could result in a *_buffer overrun*_.
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Under extreme conditions the *SAVE FITS* command could result in a *buffer overrun*.
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Fixed code with *asserts disabled*. Compiling the code with EXTRA=-DNDEBUG should now result in run times ~3% faster when averaged over the test suite, but with internal consistency checks removed.
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... | ... | @@ -187,7 +187,7 @@ The recommended syntax for running Cloudy is now |
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This will read input commands from `script.in` and write output to `script.out`.
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For more details see the [wiki:RunningC13] page.
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The way Cloudy generates its return value has been modified. Also the return value of cdDrive() has been changed from int to bool. This enables us to give a more detailed and reliable overview of what went wrong in a grid run in the *_save grid*_ output. *_For users that call Cloudy as a subroutine this implies that they need to modify their main program.*_ See the program in tsuite/programs/template.cpp for the new way of calling Cloudy. Also the parameters of the routine cdGetLineList() have been modified to enable detecting memory leaks. See Hazy 2 for further details.
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The way Cloudy generates its return value has been modified. Also the return value of cdDrive() has been changed from int to bool. This enables us to give a more detailed and reliable overview of what went wrong in a grid run in the *save grid* output. *For users that call Cloudy as a subroutine this implies that they need to modify their main program.* See the program in tsuite/programs/template.cpp for the new way of calling Cloudy. Also the parameters of the routine cdGetLineList() have been modified to enable detecting memory leaks. See Hazy 2 for further details.
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## New commands or options
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... | ... | @@ -200,18 +200,18 @@ The way Cloudy generates its return value has been modified. Also the return val |
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*set check energy every zone* command created.
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The *grid*_ command now accepts negative increments, allowing you to move from a high to a low value
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The *grid* command now accepts negative increments, allowing you to move from a high to a low value
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The *set atomic data sulphur* command has been removed.
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The *kludge option on the set dielectronic recombination* command has been *renamed mean*.
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There is a new command, *set dielectronic recombination mean scale*_, that will multiply the estimates
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There is a new command, *set dielectronic recombination mean scale*, that will multiply the estimates
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of the dielectronic
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recombination for ions with not data, by specified scale factors. This provides a simple way to judge the
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sensitivity of predictions to these uncertain rates.
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The *set dielectronic recombination Badnell print* command is *_replaced with the print recombination*_ command
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The *set dielectronic recombination Badnell print* command is *replaced with the print recombination* command
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Most *set dielectronic recombination* options have been removed since we now use the Badnell database exclusively.
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... | ... | @@ -223,7 +223,7 @@ The *set chianti levels X Y* command sets the maximum number of Chianti energy l |
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The *save cooling each* command created to indicate the contribution of each element to the total cooling.
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The *save line list* command now has a *_column option*_ to report the results in column rather than row output.
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The *save line list* command now has a *column option* to report the results in column rather than row output.
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The results are the linear quantity rather than the log.
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The *save species labels command* creates a list of the labels we use for atoms, ions, and molecules.
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... | ... | @@ -254,10 +254,9 @@ when inside the Cloudy data directory. |
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## Stellar grids and other SEDS
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We have added support for the [Rauch C/O white dwarf grid](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_C+O+Ne+Mg.html) using the *_table star rauch co wd*_ command.
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We have added support for the [Rauch C/O white dwarf grid](http://astro.uni-tuebingen.de/~rauch/TMAF/flux_C+O+Ne+Mg.html) using the *table star rauch co wd* command.
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The *table Crab command now uses the SED from Hester (2008 ARA&A).*
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The old SED, based on Davidson (1985 ARA&A) is available with the *_table Crab Davidson*_ command.
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The old SED, based on Davidson (1985 ARA&A) is available with the *table Crab Davidson* command.
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The keywords *stellar* and *nebular* have been added to the *compile stars command for Starburst99 files*. The effect is to use only the stellar or the nebular component of the interstellar radiation field, rather than the sum of the two. The latter remains the default.
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... | ... | @@ -280,7 +279,7 @@ The *Badnell dielectronic recombination rates are updated* to Abdel-Naby et al A |
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The *Badnell dielectronic and radiative recombination* database are *now used exclusively*.
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We are now using the *hybrid collisional ionization rate coefficients*_ by default.
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We are now using the *hybrid collisional ionization rate coefficients* by default.
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Hybrid means that the original rates given by Voronov, G. S. 1997, At.Data Nucl. Data Tables, 65, 1 are multiplied by a scale factor.
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This scale factor is the collisional ionization rate coefficient at the center of the discrete temperature range given by Dere, K. P. 2007, A&A, 466, 771 divided by the collisional ionization rate coefficient given by Voronov at the same temperature.
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