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NOTE:
the present 7 September 2007 version now
includes additional molecular opacity tables, as well as an
example of an interactive driver program (plus a couple
of minor bug-fixes from the 6 April 2007 version).
[As of 29 March 2007, the subroutines
include optional extension to high densities via the updated
Potekhin et al. (2006) conductive opacities, and to low
temperatures via the updated Ferguson et al. (2005)
molecular opacities.]
[As of 9 July 2018, three opacity files stored under incorrect filenames have been corrected (namely, the files 'AGS04hz_OFe.5_W95hz', 'AGS04hiCNONe_OFe.5_W95hz', and 'AGS04vhCNONe_OFe.5_W95hz' were corrected to become 'AGS04hz_OFe.5_W95', 'AGS04hiCNONe_OFe.5_W95', and 'AGS04vhCNONe_OFe.5_W95', respectively).]
Available below are a set of
Fortran subroutines
(in a downloadable plain text Fortran file), and a number of sets of
opacity files.
- These Fortran subroutines are designed to read in the
1995 OPAL astrophysical opacities (from the
OPAL opacity files "Gz???.x??" and "GN93hz"),
and to subsequently
interpolate them in metallicity as well as in temperature,
density, and mass fractions of hydrogen and of "excess" carbon and oxygen
(Z, T6, R, X, exC, exO: where R=rho/T6^3).
- Opacity effects
due to CNO variations at a given Z value (resulting from nuclear burning)
can also be included, given the CNO-varied opacity files
listed below.
- At the time the opacity files are read in, interpolation
in [O/Fe] may be performed if desired (using
"W95hz", "C95hz", "Alrd96a2", or some
other non-CO-rich OPAL opacity file that has non-zero [O/Fe]).
- Opacities appropriate to mixes other than the Grevesse and
Noels 1993 solar composition can be used, either by using the alternate opacity files listed below or by having
the Livermore OPAL page
compute a new set of opacity tables.
- A Fortran test program
is also available below, to check that things
are working correctly on your computer/compiler.
- For convenience, extension is possible
via low-temperature molecular opacities and
via high-density conductive opacities
- [Note that the
test program available further below does not presently test the molecular
and conductive opacities.]
Brief History of Program Updates:
- As of 7 September 2007, if the user asks for molecular opacities to
be included and specifies a non-zero [O/Fe] value, then the
alpha-enhanced GS98 molecular opacity tables
of Ferguson et al.
will be checked for (in preference to their S92AE table) when reading the
molecular opacities: this changes the default behavior for this
case, and can lead to slightly different low-temperature opacities when
[O/Fe] is non-zero.
- The interactive example driver program had a minor bug
prior to 5 September 2007 (and the table-creation example driver
program was not available prior to this date).
- Some versions prior to 26 August 2007 had a bug that led them to
fail to notice out-of-range input metallicity values Z (returning
spurious opacity values in some such cases); this is now fixed.
- Versions prior to 6 April 2007 had less-smooth extrapolation in
temperature and density, and thus a less-smooth switchover between OPAL
and conductive opacities (and also a minor CNO-interpolation bug, which
occurred only at a hydrogen mass fraction of X = 0.03); these
are now fixed.
- Prior to 29 March 2007, only
the Hubbard and Lampe (1969) plus Itoh et al. (1984) conductive
opacities were available [the
updated (Potekhin et al. 2006) conductive opacities
have now been added].
- Prior to 24 March 2007
(but only on or after 2 February 2007),
there was a bug yielding errors
in the Hubbard and Lampe (1969) conductive opacities; this
is now fixed.
- Prior to 2 February 2007, only
the outdated (Alexander and Ferguson 1994) molecular opacities were allowed
[the updated (Ferguson et al. 2005) molecular opacities
have now been added].
- Prior to 21 September 2006, the (optional)
switchover to conductive opacities was not handled correctly; this
is now fixed.
- Prior to 6 September 2006, no conductive or molecular
opacities were available at all.
- If you used this program to produce
unformatted (binary) opacity dumpfiles
for later use, any opacity dumpfiles produced with a program version
prior to 6 September 2006 are incompatible with later program versions
(and would have to be recomputed).
z14xcotrin21.f (1.2 Mb) |
(Full-Z:
program uses 24 Mb of internal opacity storage matrices):
Note that this version of the subroutines allows Z-interpolation over
the full available metallicity range from Z = 0.0 to 0.1 |
z14xcotrin21.f.gz (gzip-compressed to 0.24 Mb) |
z14xcotrin21.f.bz2 (bzip2-compressed to 0.19 Mb) |
z5xcotrin21.f (1.2 Mb) |
(Restricted-Z:
program uses 9.2 Mb of internal opacity storage matrices):
Allows Z-interpolation within about a factor of two of a given input metallicity
Z |
z5xcotrin21.f.gz (gzip-compressed to 0.24 Mb) |
z5xcotrin21.f.bz2 (bzip2-compressed to 0.19 Mb) |
z1xcotrin21.f (1.2 Mb) |
(Single-Z:
program uses 2.7 Mb of internal opacity storage matrices):
Allows only a single constant Z-value (Z-interpolation can be performed
only when the opacities are being read in). This version is still somewhat
more flexible than the opacity routines that are supplied on the Livermore OPAL page.
|
z1xcotrin21.f.gz (gzip-compressed to 0.24 Mb) |
z1xcotrin21.f.bz2 (bzip2-compressed to 0.19 Mb) |
z_xcotrin_example.f (0.03 Mb) |
An
example of an interactive driver program, that asks
which opacities should be read in, then asks for temperature,
density, composition values for which to compute opacities |
z_xcotrin_ZXtable.f (0.04 Mb) |
An
example of an interactive table-creation driver program,
that produces a (text-file) opacity table for a single
composition (in roughly the OPAL format) |
z_xcotrin_manual.pdf |
The
Manual as a PDF file (0.14 Mb) |
z_xcotrin_manual.ps.gz |
The
Manual
as a gzip-compressed
PostScript file (0.08 Mb, expands to 0.33 Mb) |
z_xcotrin_tst.f (7.1 Mb) |
A
test program that checks calculated opacities against stored values
(this may take a few minutes to run).
Note that, by default, binary opacity dumps are created that require at
least 40 Mb of free disk space.
|
z_xcotrin_tst.f.gz (gzip-compressed to 1.0 Mb) |
z_xcotrin_tst.f.bz2 (bzip2-compressed to 0.7 Mb) |
All of the required opacity files are available below. The OPAL
opacity files can also be obtained at the
Livermore OPAL page
(see C. A. Iglesias and F. J. Rogers 1996, Astrophysical Journal,
464, 943)
[the (optional) updated conductive and
molecular opacity files can also be obtained at the
Potekhin and
Ferguson web pages,
respectively].
- The relevant compositions for these opacity files are listed in the
manual (and in the comments to the Fortran files).
- The md5sum values [to check downloaded files] for all 77 OPAL opacity
files are listed in the plain text file
OPALmd5sum.txt
- The md5sum values for the new and old
conductive opacities [and the old (1994) molecular opacities]
are listed in the plain text file
MOLCONDmd5sum.txt
- The md5sum values for the 1705
Ferguson et al. molecular opacity files [in subdirectories as obtained from
the OPALkappa.tar files below] are listed in the plain text file
MOLSUBmd5sum.txt
- The md5sum values for each individual set
of 155 Ferguson et al. molecular opacity files can be obtained from their
table further below
OPALkappa.tar.gz |
(gzip-compressed
tar archive: 23.3 Mb, expands to 84.4 Mb) |
OPALkappa.tar.bz2 |
(bzip2-compressed
tar archive:
14.4 Mb, expands to 84.4 Mb) |
OPALtar_md5sum.txt |
a text file
containing md5sum values for these archives [to check downloads] |
GN93hz.gz |
(gzip'd
plain text: 0.32 Mb, expands to 1.17 Mb) |
(OR
plain text: 1.17 Mb) |
GN93hz |
W95hz.gz |
(gzip'd
plain text: 0.31 Mb, expands to 1.17 Mb) |
(OR
plain text: 1.17 Mb) |
W95hz |
condall06.gz |
(gzip'd
plain text: 0.05 Mb, expands to 0.13 Mb) |
(OR
plain text: 0.13 Mb) |
condall06.d |
Condopac.gz |
(gzip'd
plain text: 0.01 Mb, expands to 0.023 Mb) |
(OR
plain text: 0.023 Mb) |
Condopac |
gzip-compressed tar archives, each containing 155 plain-text
files (compressed archive size 0.6 Mb, expanding to 1.9 Mb); and corresponding
(text) md5sum-files (containing md5sum values for the individual
opacity files) |
||
f05.g93.tar.gz |
GN93
composition |
MOLf05_g93_md5sum.txt |
f05.gs98.tar.gz |
GS98
composition |
MOLf05_gs98_md5sum.txt |
f05.l03.tar.gz |
Lodders
2003 composition (similar to AGS04) |
MOLf05_l03_md5sum.txt |
f05.ags04.tar.gz |
AGS04
composition |
MOLf05_ags04_md5sum.txt |
f05.s92.tar.gz |
Seaton
1992 composition (similar to GN93) |
MOLf05_s92_md5sum.txt |
f05.s92ae.tar.gz |
Seaton
1992 alpha-enhanced: [O/Fe] = [alpha/Fe] = +0.3 |
MOLf05_s92ae_md5sum.txt |
f05.gs98-.2.tar.gz |
GS98
alpha-depleted: [O/Fe] = [alpha/Fe] = -0.2 |
MOLf05_gs98-.2_md5sum.txt |
f05.gs98+.2.tar.gz |
GS98
slightly alpha-enhanced: [O/Fe] = [alpha/Fe] = +0.2 |
MOLf05_gs98+.2_md5sum.txt |
f05.gs98+.4.tar.gz |
GS98
alpha-enhanced: [O/Fe] = [alpha/Fe] = +0.4 |
MOLf05_gs98+.4_md5sum.txt |
f05.gs98+.6.tar.gz |
GS98
strongly alpha-enhanced: [O/Fe] = [alpha/Fe] = +0.6 |
MOLf05_gs98+.6_md5sum.txt |
f05.gs98+.8.tar.gz |
GS98
extremely alpha-enhanced: [O/Fe] = [alpha/Fe] = +0.8 |
MOLf05_gs98+.8_md5sum.txt |
Alexopac.gz |
(gzip'd
plain text: 0.1 Mb, expands to 0.35 Mb) |
(OR
plain text: 0.35 Mb) |
Alexopac |
(gzip'd
plain text: 0.32 Mb, expands to 1.17 Mb): |
CNO-composition variation: | (OR
plain text: 1.17 Mb): |
GN93hz.CtoN.gz |
Almost all
the C was converted to N |
GN93hz.CtoN |
GN93hz.COtoN.gz |
Almost all
the C and O were converted to N |
GN93hz.COtoN |
GN93hz.CNOtoNe.gz |
All
the C, N, and O were converted to Ne |
GN93hz.CNOtoNe |
GS98hz.gz |
(gzip'd
plain text) |
(OR
plain text: 1.17 Mb) |
GS98hz |
GS98hz_OFe.5_W95.gz |
(gzip'd
plain text) |
(OR
plain text: 1.17 Mb) |
GS98hz_OFe.5_W95 |
(gzip'd
plain text: 0.32 Mb, expands to 1.17 Mb): |
(OR
plain text: 1.17 Mb): |
GS98hz.CtoN.gz |
GS98hz.CtoN |
GS98hz.COtoN.gz |
GS98hz.COtoN |
GS98hz.CNOtoNe.gz |
GS98hz.CNOtoNe |
AGS04hz.gz |
(gzip'd
plain text) |
(OR
plain text: 1.17 Mb) |
AGS04hz |
AGS04hz_OFe.5_W95.gz |
(gzip'd
plain text) |
(OR
plain text: 1.17 Mb) |
AGS04hz_OFe.5_W95 |
(gzip'd
plain text: 0.32 Mb, expands to 1.17 Mb): |
(OR
plain text: 1.17 Mb): |
AGS04hz.CtoN.gz |
AGS04hz.CtoN |
AGS04hz.COtoN.gz |
AGS04hz.COtoN |
AGS04hz.CNOtoNe.gz |
AGS04hz.CNOtoNe |
(gzip'd
plain text: 0.32 Mb, expands to 1.17 Mb): |
Ne factor |
Z/X:sun |
(OR
plain text: 1.17 Mb): |
AGS04x15Ne.gz |
1.5 |
0.01725 |
AGS04x15Ne |
AGS04x2Ne.gz |
2.0 |
0.01794 |
AGS04x2Ne |
AGS04x25Ne.gz |
2.5 |
0.01863 |
AGS04x25Ne |
AGS04x3Ne.gz |
3.0 |
0.01933 |
AGS04x3Ne |
AGS04hiCNONe.gz |
(gzip'd
plain text) |
(OR
plain text: 1.17 Mb) |
AGS04hiCNONe |
AGS04hiCNONe_OFe.5_W95.gz |
(gzip'd
plain text) |
(OR
plain text: 1.17 Mb) |
AGS04hiCNONe_OFe.5_W95 |
(gzip'd
plain text: 0.32 Mb, expands to 1.17 Mb): |
(OR
plain text: 1.17 Mb): |
AGS04hiCNONe.CtoN.gz |
AGS04hiCNONe.CtoN |
AGS04hiCNONe.COtoN.gz |
AGS04hiCNONe.COtoN |
AGS04hiCNONe.CNOtoNe.gz |
AGS04hiCNONe.CNOtoNe |
(gzip'd
plain text: 0.32 Mb, expands to 1.17 Mb): |
Ne factor |
Z/X:sun |
(OR
plain text: 1.17 Mb): |
AGS04hiCNOx15Ne.gz |
1.5 |
0.01888 |
AGS04hiCNOx15Ne |
AGS04hiCNOx2Ne.gz |
2.0 |
0.01965 |
AGS04hiCNOx2Ne |
AGS04hiCNOx25Ne.gz |
2.5 |
0.02043 |
AGS04hiCNOx25Ne |
AGS04hiCNOx3Ne.gz |
3.0 |
0.02121 |
AGS04hiCNOx3Ne |
AGS04vhCNONe.gz |
(gzip'd
plain text) |
(OR
plain text: 1.17 Mb) |
AGS04vhCNONe |
AGS04vhCNONe_OFe.5_W95.gz |
(gzip'd
plain text) |
(OR
plain text: 1.17 Mb) |
AGS04vhCNONe_OFe.5_W95 |
(gzip'd
plain text: 0.32 Mb, expands to 1.17 Mb): |
(OR
plain text: 1.17 Mb): |
AGS04vhCNONe.CtoN.gz |
AGS04vhCNONe.CtoN |
AGS04vhCNONe.COtoN.gz |
AGS04vhCNONe.COtoN |
AGS04vhCNONe.CNOtoNe.gz |
AGS04vhCNONe.CNOtoNe |
(gzip'd
plain text: 0.32 Mb, expands to 1.17 Mb): |
Ne factor |
Z/X:sun |
(OR
plain text: 1.17 Mb): |
AGS04vhCNOx15Ne.gz |
1.5 |
0.02070 |
AGS04vhCNOx15Ne |
AGS04vhCNOx2Ne.gz |
2.0 |
0.02158 |
AGS04vhCNOx2Ne |
AGS04vhCNOx25Ne.gz |
2.5 |
0.02245 |
AGS04vhCNOx25Ne |
AGS04vhCNOx3Ne.gz |
3.0 |
0.02332 |
AGS04vhCNOx3Ne |