ATLAS12 for LINUX 
 
The KURUCZ original code for VMS works also in unix with intel fortran.
http://kurucz.harvard.edu/programs/atlas12 


ATLAS12 for Linux for g_fortran:-- NOVEMBER 2017--
atlas12.for 

compile: gfortran -fno-automatic -w -o atlas12.exe atlas12.for

To run  ATLAS12  type:

source asunkat12tot.com
asunkat12tot.com

fclowlines.bin and fchilines.bin are available at:
http://kurucz.harvard.edu/linelists/linescd/

tioschwenke.bin is available at:
http://kurucz.harvard.edu/molecules/tio 

h2ofasfix.bin is available at:
http://kurucz.harvard.edu/molecules/h2o 


The file diatomics.pck is the binary of diatomics.asc which is available in:
http://kurucz.harvard.edu/molecules/OLDandNEW 

To convert diatomics.asc in binary form:
diatomicspack.for 
diatomicspack.com 
diatomicspack does not convert AlO and NaH in binary form. Work in progress. 

The file nltelines.bin is the binary of the file nltelines.asc which is available in:
http://kurucz.harvard.edu/linelists/linescd/
To convert nltelines.asc in binary form:
nltelinesasctobin.for 
nltelinesasctobin.com 

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ATLAS12 for Linux for INTEL fortran:--MARCH 2012:


atlas12_mar12.for intel fortran version
compile: ifort -double-size 64 -save -o atlas12_mar12.exe atlas12_mar12.for

       
MORE DETAILS:

This example shows how to compute an ATLAS12 model with parameters:
SCALED SOLAR abundance [M/H]=-1.0, but with Mg=[-1.0+0.3], Teff=5500K, logg=4.6, vturb=1.23 km/s
The ATLAS12 model assumes Anders & Grevesse (1989) solar abundances,
while the ATLAS9 input model was computed using the Grevesse & Sauval (1998)
solar abundances.This implies that in addition to the Mg abundance also 
several abundances of the ATLAS9 input model have to be changed by means of 
ABUNDANCE CHANGE cards.

To run the ATLAS12 model type:

source am10t5500g46k123MgP03_linux.com

where am10t5500g46k123MgP03_linux.com is:

ln -s molecules.dat fort.2
ln -s am10t5500g45k1odfnew.dat fort.3        !!!  ATLAS9 (or ATLAS12) input model 
ln -s http://kurucz.harvard.edu/linelists/linescd fclowlines.bin fort.11   !!fclowlinws.bin runs under linux--lowlines.bin does not
ln -s http://kurucz.harvard.edu/linelists/linescd fchighlines.bin fort.11  !!fchighlines.bin runs under linux--highlines.bin does not
ln -s diatomicsiwl.bin  fort.31
ln -s http://kurucz.harvard.edu/molecules/tio/ tiosschwenke.bin fort.41
ln -s http://kurucz.harvard.edu/molecules/h2o/ h2ofastfix.bin fort.51
./atlas12.exe<am10t5500g46k123at12a.out
MOLECULES ON
READ MOLECULES
READ PUNCH
READ LINES
CONVECTION OVER 1.25 0 36
ITERATIONS 1 PRINT 1 PUNCH 0
ABUNDANCE CHANGE 3 -10.88
ABUNDANCE CHANGE 4 -10.89
ABUNDANCE CHANGE 5 -9.44
ABUNDANCE CHANGE 6 -3.48
ABUNDANCE CHANGE 7 -3.99
ABUNDANCE CHANGE 8 -3.11
ABUNDANCE CHANGE 10 -3.95
ABUNDANCE CHANGE 12 -4.16
ABUNDANCE CHANGE 16 -4.83
ABUNDANCE CHANGE 18 -5.48
ABUNDANCE CHANGE 19 -6.82
ABUNDANCE CHANGE 21 -8.94
ABUNDANCE CHANGE 22 -7.05
ABUNDANCE CHANGE 26 -4.53
ABUNDANCE CHANGE 36 -8.81
ABUNDANCE CHANGE 38 -9.14
ABUNDANCE CHANGE 40 -9.54
ABUNDANCE CHANGE 48 -10.18
ABUNDANCE CHANGE 49 -10.58
ABUNDANCE CHANGE 54 -9.81
ABUNDANCE CHANGE 55 -10.92
ABUNDANCE CHANGE 57 -10.82
ABUNDANCE CHANGE 58 -10.49
ABUNDANCE CHANGE 62 -11.04
ABUNDANCE CHANGE 65 -11.94
ABUNDANCE CHANGE 66 -10.94
ABUNDANCE CHANGE 71 -11.28
ABUNDANCE CHANGE 73 -11.91
ABUNDANCE CHANGE 75 -11.77
ABUNDANCE CHANGE 80 -10.85
ABUNDANCE CHANGE 82 -10.19
ABUNDANCE CHANGE 90 -11.92
ABUNDANCE CHANGE 92 -12.51
BEGIN
END
EOF
mv fort.12 sellinm10t5500g46k123.bin
rm fort.*
ln -s am10t5500g45k1odfnew.dat fort.3        !!!  The same ATLAS9 (or ATLAS12) input model as before 
ln -s molecules.dat fort.2
ln -s nltelines.bin fort.19
ln -s sellinm10t5500g46k123.bin fort.12
./atlas12.exe<am10t5500g46k123at12b.out
MOLECULES ON
READ MOLECULES
READ PUNCH
TITLE ATLAS12 
OPACITY ON LINES
OPACITY ON XLINES
CONVECTION OVER 1.25 0 36
ITERATIONS 45
PRINT 1 0 0 0 0 0 0 0 0 0 0 0 0 0 1 0 0 0 0 0 0 0 0 0 0 0 0 0 0 1 0 0 0 0 0 0 0 0 0 0 0 0 0 0 1 
PUNCH 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 1
SCALE MODEL 72 -6.875 0.125 5500. 4.6
VTURB 1.23E+05
ABUNDANCE CHANGE 3 -10.88
ABUNDANCE CHANGE 4 -10.89
ABUNDANCE CHANGE 5 -9.44
ABUNDANCE CHANGE 6 -3.48
ABUNDANCE CHANGE 7 -3.99
ABUNDANCE CHANGE 8 -3.11
ABUNDANCE CHANGE 10 -3.95
ABUNDANCE CHANGE 12 -4.16
ABUNDANCE CHANGE 16 -4.83
ABUNDANCE CHANGE 18 -5.48
ABUNDANCE CHANGE 19 -6.82
ABUNDANCE CHANGE 21 -8.94
ABUNDANCE CHANGE 22 -7.05
ABUNDANCE CHANGE 26 -4.53
ABUNDANCE CHANGE 36 -8.81
ABUNDANCE CHANGE 38 -9.14
ABUNDANCE CHANGE 40 -9.54
ABUNDANCE CHANGE 48 -10.18
ABUNDANCE CHANGE 49 -10.58
ABUNDANCE CHANGE 54 -9.81
ABUNDANCE CHANGE 55 -10.92
ABUNDANCE CHANGE 57 -10.82
ABUNDANCE CHANGE 58 -10.49
ABUNDANCE CHANGE 62 -11.04
ABUNDANCE CHANGE 65 -11.94
ABUNDANCE CHANGE 66 -10.94
ABUNDANCE CHANGE 71 -11.28
ABUNDANCE CHANGE 73 -11.91
ABUNDANCE CHANGE 75 -11.77
ABUNDANCE CHANGE 80 -10.85
ABUNDANCE CHANGE 82 -10.19
ABUNDANCE CHANGE 90 -11.92
ABUNDANCE CHANGE 92 -12.51
BEGIN 
END
EOF
mv fort.7  am10t5500g46k123at12MgP03.dat 
rm fort.*



In the above command file:

"molecules.dat" are molecular data for computing molecular populations
"fclowlines.bin" are lines of all elements from first 5 stages of ionization, with exception for the lines of 
HI, HeI, HeII, CI, CII, OI, NaI, MgI, MgII, AlI, SiI, SiII, KI, CaI, CaII, which are collected in "nltelines.bin"
"fchighlines.bi" are lines of elements with ionization stages higher than 5.
"diatomicsiwl.bin" are lines from diatomic molecules ordered by increasing wavelength
"tioschwenke.bin" are TiO lines from Schwenke
"h2ofastfix.bin" are H2O lines from Partridge & Schwenke