New in Next Release
This page summarizes all major changes and improvements to Cloudy that will be included in the next release. You may also view the HotFixes and KnownProblems pages, or return to the main RevisionHistory page.
Caveats
Changes to command parser
All option on save line intensities command to save all lines, including those with zero intensity.
Print Voigt a=xxx command created.
set check energy every zone command created.
The grid command now accepts negative increments, allowing you to move from a high to a low value.
The set atomic data sulphur command has been removed.
The kludge option on the set dielectronic recombination command has been renamed mean.
There is a new command, set dielectronic recombination mean scale, that will multiply the estimates of the dielectronic recombination for ions with not data, by specified scale factors. This provides a simple way to judge the sensitivity of predictions to these uncertain rates.
The set dielectronic recombination Badnell print command is replaced with the print recombination command.
Most set dielectronic recombination options have been removed since we now use the Badnell database exclusively.
The abundances GASS10 command allows Cloudy to use the solar abundances from Grevesse et al. (2010).
The set collisional ionization X command has two options: Dima or Hybrid.
The set chianti levels X Y command sets the maximum number of Chianti energy levels to use for iron species, X, and all other species, Y.
The save cooling each command created to indicate the contribution of each element to the total cooling.
The save line list command now has a column option to report the results in column rather than row output. The results are the linear quantity rather than the log.
Grain physics
Two new refractive index files ph3n.rfi and ph3c.rfi have been added. These produce the opacities of neutral and charged PAHs, resp., following the prescription of Draine, B.T. & Li, A., 2007 ApJ, 657, 810. These files are temporary and will eventually be replaced by a single file that self-consistently determines the opacity from the actual charge of the PAH during execution. This however requires substantial changes to the code that are not yet complete. To produce opacity files from these refractive index files, you can e.g. use:
compile grains "ph3n.rfi" "ab08.szd" 10 compile grains "ph3c.rfi" "ab08.szd" 10
when inside the Cloudy data directory.
Stellar grids and other SEDS
We have added support for the Rauch C/O white dwarf grid using the table star rauch co wd command.
The table Crab command now uses the SED from Hester (2008 ARA&A). The old SED, based on Davidson (1985 ARA&A) is available with the table Crab Davidson command.
Improved physics and numerical methods
Cosmic ray background ionization rate updated to Indriolo+07.
Ryan add quadrupole transitions for He I. TO DO
We have added 31 new molecules from the CDMS and JPL molecular spectroscopy databases.
The dielectronic and radiative recombination databases have been updated to the April 2011 versions on the Badnell web site. This includes the updated Argon isoelectronic sequence (Nikolic et al, 2010, A&A 516, A97).
The Badnell dielectronic and radiative recombination database are now used exclusively.
We are now using the hybrid collisional ionization rate coefficients by default. 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. 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.
The Chianti line database is now used for Fe VI through Fe XXIV and select species between phosphorus and zinc.
Enhancements for time-dependent cases
Other changes
Solar Abundances updated to Grevesse et al. (2010).
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Attachments
- O3LineRatio.jpg (53.7 kB) - added by gary 5 years ago.
