NOTE: some FORTRAN files were modified at CDS to ensure an edition
of the result to the standard output (required for the usage behind
a HTTP server). The original files were renamed xxx_ori.f
================================================================================

drwxr-xr-x 3 10075 10075   4096 Jul 12  2017 [Up]
drwxr-xr-x 2 10075 10075   4096 Apr 25  2009 [TAR file]
-r--r--r-- 1 10075 10075    639 Apr 25  2009 Makefile
-r--r--r-- 1 10075 10075 302323 Mar 30  1998 OVS0001
-r--r--r-- 1 10075 10075 321125 Mar 30  1998 OVS0003
-r--r--r-- 1 10075 10075 328235 Mar 30  1998 OVS001
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-r--r--r-- 1 10075 10075 361573 Mar 30  1998 OVS03
-r--r--r-- 1 10075 10075   7688 Apr 25  2009 README
-r--r--r-- 1 10075 10075   7413 Aug 19  1998 README.ori
-r--r--r-- 1 10075 10075 149001 Mar 25  1998 STD0001
-r--r--r-- 1 10075 10075 155795 Mar 25  1998 STD0003
-r--r--r-- 1 10075 10075 158165 Mar 24  1998 STD001
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-r--r--r-- 1 10075 10075 354752 Mar 23  1998 STD03
-r--r--r-- 1 10075 10075 320136 Dec 12  1997 UBVRI.Kur
-r--r--r-- 1 10075 10075 320136 Dec 12  1997 UBVRI.LBC
-r--r--r-- 1 10075 10075  28206 Mar 18  1998 ZAMS0001
-r--r--r-- 1 10075 10075  28206 Mar 18  1998 ZAMS0003
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-r--r--r-- 1 10075 10075    438 Mar 19  1998 indx.f
-r--r--r-- 1 10075 10075   1433 Mar 19  1998 intplz.f
-r--r--r-- 1 10075 10075   1836 Apr 25  2009 iso.f
-r--r--r-- 1 10075 10075   1495 Aug 19  1998 iso_ori.f
-r--r--r-- 1 10075 10075   6744 Mar 19  1998 isochr.f
-r--r--r-- 1 10075 10075    453 Aug 19  1998 makefile.ori
-r--r--r-- 1 10075 10075   4604 Mar 24  1998 mkgrid.f
-r--r--r-- 1 10075 10075   2993 Aug 19  1998 rdgrid.f
-r--r--r-- 1 10075 10075   2400 Mar 19  1998 track.f
-r--r--r-- 1 10075 10075   1627 Apr 25  2009 trk.f
-r--r--r-- 1 10075 10075   1264 Aug 19  1998 trk_ori.f
-r--r--r-- 1 10075 10075   2302 Aug 19  1998 ubvcol.f


 Beginning of  README :
NOTE: some FORTRAN files were modified at CDS to ensure an edition
of the result to the standard output (required for the usage behind
a HTTP server). The original files were renamed xxx_ori.f
================================================================================

Contents:
--------
This package contains 3 sets of files that allow the construction of
isochrones for arbitrary age and metallicity: 
(1) evolution tracks and ZAMS models, as described in the paper by 
    Pols, Schroder, Tout, Hurley & Eggleton (1998, MNRAS, 298, 525).
(2) synthetic bolometric corrections and UBVRI colours, for the conversion
    of (L,Teff) to broadband magnitudes and colours.
(3) subroutines for reading the above data and interpolating tracks and 
    constructing isochrones.

file:			description:

OVS0001 ... OVS03	evolution tracks with `overshooting', delta(OV)=0.12,
			for Z=0.0001 to 0.03 (7 files), M=0.5...50 Msol
STD0001 ... STD03	'standard' evolution tracks, delta(OV)=0,
			for Z=0.0001 to 0.03 (7 files), M=0.5...2.0 Msol
			(Z<=0.004) or M=0.5...40 Msol (Z>=0.01)
ZAMS0001 ... ZAMS03	ZAMS models for Z=0.0001 to 0.03 (7 files),
			M=0.1...100 Msol
UBVRI.Kur		table of synthetic BC and UBVRI colours, from Kurucz 
			model atmospheres (1992, IAU Symp 149, p.225)
UBVRI.LBC		empirically corrected version of the above, from
			Lejeune, Cuisinier & Buser (1997, A&AS 125, 229)
indx.f ... ubvcol.f	9 FORTRAN77 subroutines for grid assembly, track
			interpolation and isochrone construction
makefile		makefile for compilation

Introduction: 
------------ 
Two sets of evolution tracks are provided, one (OVS) computed with extended
mixing or `overshooting', the other (STD) without. As discussed in our paper
(cited above), empirical tests show that the OVS tracks should be preferred
for M >= 1.6 Msol, but that the assumed amount of overshooting is too large
for lower masses. For M <= 1.0 Msol, however, both sets of models are
essentially the same. For consistency, it would be best to use the OVS models
over the entire range, but this may lead to an erroneus location of the
main-sequence hook in the mass range 1.0 - 1.6 Msol. Perhaps the best
compromise would be to interpolate in this mass range by using a `hybrid' 
grid as described below.

Each stellar model in the grids is represented by one line of information,
i.e.: [column 1] equivalent model number (referring to the evolutionary
state, as described in the paper), [2] actual model number in output of the
evolution run, [3] age (yrs) , [4] log of effective temperature (K), [5] log
luminosity (Lsun), [6] log radius (Rsun), [7] helium core mass (Msun; defined
as the mass shell where X=0.1), [8] carbon/oxygen core mass (Msun; mass shell
where Y=0.1), [9] dimesionless moment of inertia k^2 = I/(MR^2), [10] log of
central temerature (K), [11] log of central density (g cm^-3), [12-16]
central mass fractions of H1, He4, C12, N14 and O16, [17-21] surface mass
fractions of the same.

Finally, it should be kept in mind that, if the isochrones will be used for 
comparison with broadband magnitudes and colours, the colour conversion is 
an important intermediate step and a source of uncertainty, especially for 
cool stars. Two tables are provided for this conversion, without warranty.
In the present version, the empirically corrected Kurucz tables are read from
file UBVRI.LBC. If preferred, this can be changed to read the original Kurucz
tables, but in principle any other method can be used to make the colour 
conversion.

Instructions for use: 
-------------------- 
To use the provided subroutines for interpolating evolution tracks and
constructing isochrones, first the appropriate evolution grid must be
assembled from the data files. This is done with the program MKGRID, which
is compiled with the command `make mkgrid'. You can specify upon running the
program:

* whether the STD models, the OVS models or a hybrid (HYB) grid is to be
  used. The HYB grid is assembled from OVS models for M >= 1.6 Msun, and STD
  models for M <= 1.4 Msun up to the He flash. For post He-flash models, OVS
  models are used for all masses (because all such low-mass models contain a
  0.5 Msun He core and their physical structure is very similar);

* the required range of metallicities and masses;

* the amount of detail required: only global properties (up to column 6
  above), interior structure data (up to column 11), composition data (all
  columns).

MKGRID creates the files EVOLGRID and ZAMSGRID. The last specifications are
to avoid creating, and having to read, very large tables, when the
application requires only a limited M or Z range or a limited amount of
detail. For example, the subroutines for the construction of isochrones only
use the global properties.

At installation of the other routines, the values of character string DIREC
in subroutines RDGRID and RDUBVI should be changed to the appropriate
directory paths where the data files are placed. In the application program,
these two subroutines should be called first to read the data. RDGRID returns
the type of grid it has read from EVOLGRID as a 3-letter code.

Subroutine TRACK has two input arguments: MLOG = log(M/Msun) and ZLOG = 
log(Z/0.02). It first calls subroutine INTPLZ to interpolate in Z; if many
tracks are interpolated for a single Z value it is much more efficient to 
call INTPLZ outside TRACK. The output is stored in COMMON block TRKDAT,
i.e. for each equivalent model number: age, log Teff, log L, log R, mass, M_V
(abs.vis.magnitude), U-B, B-V, V-R, V-I, and the total number of points. 

Subroutine ISOCHR has four input arguments: AJ = age (in yrs), ZLOG = 
log(Z/0.02), MLMIN = minimum log(mass/Msol), MLMAX = maximum log(mass/Msol).
The last two parameters allow computation over a limited mass range; making
MLMIN very small and MLMAX very large produces an isochrone over the whole
mass range of the evolution grid.
The output is stored in COMMON block ISODAT, i.e. for each point along the
isochrone: zero-age mass, actual mass, log Teff, log L, log R, M_V, U-B, B-V,
V-R, V-I, equivalent model number, and the total number of points. (The
equivalent model number referes to the evolutionary status.)

Examples:
--------
The programs TRK and ISO serve as examples of the kind of output generated by
TRACK and ISOCHR respectively, as well as of how the subroutines can be
implemented in other programs. To use them, compile the codes with the
commands 'make trk' and `make iso'.

Both programs require 2 input arguments on the command line. For TRK, specify
M/Msun and Z, e.g.:

> trk 1.63 0.0072
produces an evolution track for 1.63 Msun and Z=0.0072.

For ISO, specify log(age) and [Fe/H], e.g.:

> iso 9.0 -0.22
produces an isochrone for 10^9 yrs with [Fe/H] = -0.22.

Notes:
-----
Please note the following incompletenesses:

* At present no mass loss is taken into account, but it can be included in a 
  simplified way for giants. I hope to modify the code to include this in the
  near future.
* The tracks usually extend up to the start of double-shell burning, i.e. 
  the start of the TP-AGB. Some tracks extend further, but not always to the
  same equivalent point, so that the interpolation beyond the early-AGB
  (model 129) can be a bit erratic. However, these late-AGB models are very
  simplified in any case because they do not include thermal pulses.
* The UBVRI tables only extend down to Teff = 3500 K. The code extrapolates
  to lower temperatures, leading to (probably) erroneous results for the M_V
  and colours of the coolest models. Lejeune et al also give BC and colours 
  for M giants and M dwarfs but these have not (yet) been incorporated in 
  the present tables.