... | ... | @@ -19,7 +19,7 @@ These have been included in the C07.02.02 service release. |
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----
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The *_punch hydrogen ionization*_ command can cause a floating point exception. The problem can be fixed by altering line 1694 of punch_do.cpp as follows:
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The *punch hydrogen ionization* command can cause a floating point exception. The problem can be fixed by altering line 1694 of punch_do.cpp as follows:
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```
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fref/MAX2(1e-37,fout),
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... | ... | @@ -164,7 +164,7 @@ Thanks to Bryan Armentrout for pointing out this issue. 2007 Sep 4. |
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[Unix patch](http://data.nublado.org/cloudy_releases/c07_02/hotfixes/)
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*Only one punch opacity command can be used in a given input stream*_ since all flavors of the punch opacity commands use the same variables. The fix involves several changes to the source and is included in R1286 of the C07.02 branch. It will be included in the next service release. Or place the patch file patch3 in the source directory and apply the patch, as described on the PatchFiles page. Thanks to Orly Gnat for reporting this problem. 2007 July 20.
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*Only one punch opacity command can be used in a given input stream* since all flavors of the punch opacity commands use the same variables. The fix involves several changes to the source and is included in R1286 of the C07.02 branch. It will be included in the next service release. Or place the patch file patch3 in the source directory and apply the patch, as described on the PatchFiles page. Thanks to Orly Gnat for reporting this problem. 2007 July 20.
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... | ... | @@ -235,7 +235,7 @@ This fix is in r1197 on the mainline and is merged into the c07.02 branch in r11 |
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-----
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Certain models that include *_the large model of the H,,2,, molecule will have trouble finding an initial solution*_ if a mix of electrons, protons, hydrogen atoms, and molecules are all present. This occurs in cosmic ray heated / ionized conditions. The problem is caused by the near perfect cancellation between very large heating and cooling terms due to collisions within X. The solution is to delay including X collisional heating / cooling until after search phase has found the rough initial temperature. The fix is to add the following to the end of routine H2_Cooling in file mole_h2.cpp. At line 3751 add these two lines:
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Certain models that include *the large model of the H,,2,, molecule will have trouble finding an initial solution* if a mix of electrons, protons, hydrogen atoms, and molecules are all present. This occurs in cosmic ray heated / ionized conditions. The problem is caused by the near perfect cancellation between very large heating and cooling terms due to collisions within X. The solution is to delay including X collisional heating / cooling until after search phase has found the rough initial temperature. The fix is to add the following to the end of routine H2_Cooling in file mole_h2.cpp. At line 3751 add these two lines:
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```
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if( conv.lgSearch )
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... | ... | @@ -246,7 +246,7 @@ The fix is included in r1176 on the mainline and is merged into the C07.02 branc |
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-----
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In prt_columns.cpp, there was *_an implicit assumption that there could not be a stage with an insignificant column between two stages with significant columns*_. So the insignificant column was used as a sentinel that the rest of the columns did not need to be printed. The assumption is not valid. The easy fix is to comment out line 73, so that it looks like this:
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In prt_columns.cpp, there was *an implicit assumption that there could not be a stage with an insignificant column between two stages with significant columns*. So the insignificant column was used as a sentinel that the rest of the columns did not need to be printed. The assumption is not valid. The easy fix is to comment out line 73, so that it looks like this:
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/* lgHIT = true; */
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... | ... | @@ -262,11 +262,11 @@ The fix causes no botches in the test suite. |
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-----
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Photoexcitation of upper levels of split ground terms by the UV radiation field is included using the "level2 lines", a large set of optically allowed transitions that D. Verner brought in from the Opacity Project. This level2 line pumping will not be included if the "no level2 lines" command is entered, since these lines are not computed. The code will *_no longer print column densities of excited levels if the level2 lines are disabled*_.
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Photoexcitation of upper levels of split ground terms by the UV radiation field is included using the "level2 lines", a large set of optically allowed transitions that D. Verner brought in from the Opacity Project. This level2 line pumping will not be included if the "no level2 lines" command is entered, since these lines are not computed. The code will *no longer print column densities of excited levels if the level2 lines are disabled*.
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-----
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The *set atomic data* command now has the option *sulphur DR* to change the treatment of S dielectronic recombination. This change was merged into the C07.02.01 release. The guesses which are used when no DR data are available are now the mean of the logs of the DR rates. This is better due to the large dispersion in rate coefficients. Accurate DR rates do not now exist for low stages of ionization of S at photoionization temperatures. The relative [S III] / [S II] ratio is an important diagnostic indicator of conditions in many nebulae. This ratio depends on the DR rates chosen. This command changes the DR rates assumed for the lowest four ionization stages of S. The default, which can also be set with the keyword *mix*, is to use the larger of the Badnell (1991; ApJ, 379, 356 ) or guessed rates. The keyword *pure*_ says to use only the Badnell rates. The keyword *_scale*_ says to use scaled oxygen DR rates. In this case one to four scale factors, one for each ionization stage, will be parsed off the command line. If fewer than four numbers occur then the last number entered will be used for the missing scale factors. The DR rate for ions of S will be equal to the DR rate for the same ionization stage of O multiplied by its scale factor.
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The *set atomic data* command now has the option *sulphur DR* to change the treatment of S dielectronic recombination. This change was merged into the C07.02.01 release. The guesses which are used when no DR data are available are now the mean of the logs of the DR rates. This is better due to the large dispersion in rate coefficients. Accurate DR rates do not now exist for low stages of ionization of S at photoionization temperatures. The relative [S III] / [S II] ratio is an important diagnostic indicator of conditions in many nebulae. This ratio depends on the DR rates chosen. This command changes the DR rates assumed for the lowest four ionization stages of S. The default, which can also be set with the keyword *mix*, is to use the larger of the Badnell (1991; ApJ, 379, 356 ) or guessed rates. The keyword *pure* says to use only the Badnell rates. The keyword *scale* says to use scaled oxygen DR rates. In this case, one to four scale factors, one for each ionization stage, will be parsed off the command line. If fewer than four numbers occur then the last number entered will be used for the missing scale factors. The DR rate for ions of S will be equal to the DR rate for the same ionization stage of O multiplied by its scale factor.
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-----
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