Changes between Version 170 and Version 171 of NextRelease


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Timestamp:
2012-10-08T22:45:30Z (5 years ago)
Author:
Gary J. Ferland
Comment:

empty NextRelease page

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  • NextRelease

    v170 v171  
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    6 == Caveats ==
    7 
    8 '''''The -p | -r syntax is now mandatory for all grid and optimizer runs.''''' This was already required for MPI runs, but is now needed for non-MPI runs as well. This change allows better error recovery in non-MPI grid runs. For other types of Cloudy runs the syntax remains unchanged, though the -p | -r syntax can be used there as well. For grid and optimizer runs this is the correct syntax:
    9 
    10 {{{
    11 non-MPI runs:
    12 
    13 /path/to/cloudy.exe [ -p | -r ] <prefix>
    14 
    15 MPI runs:
    16 
    17 mpirun -np <n> /path/to/cloudy.exe [ -p | -r ] <prefix>
    18 }}}
    19 
    20 where {{{<prefix>}}} is the name of the input file with the {{{.in}}} extension removed.
    21 
    22 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.
    23 
    246== New commands or options ==
    257
    26 '''''Cloudy has a new command line flag -h.''''' If you type {{{cloudy.exe -h}}} you will get an overview of all supported command line flags.
    27 
    28 '''''All option on save line intensities command''''' to save all lines, including those with zero intensity.
    29 
    30 '''''Print Voigt a=xxx''''' command created.
    31 
    32 '''''set check energy every zone''''' command created.
    33 
    34 The '''''grid''''' command now accepts negative increments, allowing you to move from a high to a low value.
    35 
    36 The '''''set atomic data sulphur''''' command has been removed.
    37 
    38 The '''''kludge option on the set dielectronic recombination''''' command has been '''''renamed mean'''''.
    39 
    40 There is a new command, '''''set dielectronic recombination mean scale''''', that will multiply the estimates
    41 of the dielectronic
    42 recombination for ions with not data, by specified scale factors.  This provides a simple way to judge the
    43 sensitivity of predictions to these uncertain rates.
    44 
    45 The ''''' set dielectronic recombination Badnell print''''' command is '''''replaced with the print recombination''''' command.
    46 
    47 Most ''''' set dielectronic recombination''''' options have been removed since we now use the Badnell database exclusively.
    48 
    49 The ''''' abundances GASS10 ''''' command allows Cloudy to use the solar abundances from Grevesse et al. (2010).
    50 
    51 The ''''' set collisional ionization X ''''' command has two options: Dima or Hybrid.
    52 
    53 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.
    54 
    55 The '''''save cooling each''''' command created to indicate the contribution of each element to the total cooling.
    56 
    57 The '''''save line list''''' command now has a '''''column option''''' to report the results in column rather than row output. 
    58 The results are the linear quantity rather than the log.
    59 
    60 The '''''save species labels command''''' creates a list of the labels we use for atoms, ions, and molecules.
    61 
    62 The '''''Chianti, Stout, and Lamda databases are now controlled by the atom command'''''.  Adjust their use with atom Chianti, atom Stout, and atom Lamda.
    63 
    64 The '''''save line data command accepts the units option'''''.
    65 
    66 The '''''range option''''' on the save fine optical depths, save fine opacity, and save fine continuum commands now
    67 '''''recognizes the units option'''''.
    68 
    69 The '''''set electron fraction command sets the electron density to a fraction of the hydrogen density'''''.
    708
    719== Grain physics ==
    7210
    73 '''''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:
    74 
    75 {{{
    76 compile grains "ph3n.rfi" "ab08.szd" 10
    77 compile grains "ph3c.rfi" "ab08.szd" 10
    78 }}}
    79 
    80 when inside the Cloudy data directory.
    8111
    8212== Stellar grids and other SEDS ==
    8313
    84 We have added support for the [http://astro.uni-tuebingen.de/~rauch/TMAF/flux_C+O+Ne+Mg.html Rauch C/O white dwarf grid] using the '''''table star rauch co wd''''' command.
    85 
    86 The '''''table Crab command now uses the SED from Hester (2008 ARA&A).''''' 
    87 The old SED, based on Davidson (1985 ARA&A) is available with the table Crab Davidson command.
    88 
    89 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.
    90 
    9114== Improved physics and numerical methods ==
    92 
    93 '''''Cosmic ray background ionization rate updated''''' to
    94 [http://cdsads.u-strasbg.fr/abs/2007ApJ...671.1736I Indriolo+07].
    95 
    96 Ryan add quadrupole transitions for He I.  TO DO
    97 
    98 We have added '''''31 new molecules''''' from the [http://www.astro.uni-koeln.de/cdms/entries CDMS] and [http://spec.jpl.nasa.gov/ftp/pub/catalog/catdir.html JPL] molecular spectroscopy databases.
    99 
    100 The '''''dielectronic and radiative recombination databases have been updated''''' to the April 2011 versions on the Badnell web site.
    101 This includes the updated Argon isoelectronic sequence (Nikolic et al, 2010, A&A 516, A97).
    102 
    103 The '''''Badnell dielectronic recombiantion rates are updated''''' to Abdel-Naby et al A&A v537, A40 (2012).  This does the 13 electron iso sequence.  Lines of S IV and S III are affected.
    104 
    105 The '''''Badnell dielectronic and radiative recombination''''' database are '''''now used exclusively'''''.
    106 
    107 We are now using the '''''hybrid collisional ionization rate coefficients''''' by default.
    108 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.
    109 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.
    110 
    111 The '''''Chianti''''' line database is now '''''used for Fe VI through Fe XXIV and select species between phosphorus and zinc'''''.
    11215
    11316== Enhancements for time-dependent cases ==
     
    11518
    11619== Other changes ==
    117 '''''Solar Abundances''''' updated to Grevesse et al. (2010).
    118 
    119 '''''Mean line optical depths are now printed in the main output.'''''  Previously we had printed line center optical depths.
    12020
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