Naming scheme:
Suffix
M01 = [-0.1} log metal abundance relative to solar
P00 = [+0.0] solar abundances from Anders and Grevesse ( )
P05 = [+0.5] log metal abundance relative to solar
A = alpha enchanced, the alpha-process elements (O, Ne, Mg, Si,
S, Ar, Ca, and Ti) enhanced by +0.4 in the log and Fe -4.53
B = alpha enchanced, the alpha-process elements (O, Ne, Mg, Si,
S, Ar, Ca, and Ti) enhanced by +1.0 in the log and Fe -4.53
F = solar Fe abundance reduced to current value -4.51
HE = He number fraction specified in per cent
Y = He mass fraction specified in per cent
NOVER = models with no convective overshooting computed by Fiorella
Castelli [castelli@ts.astro.it] in Trieste. The convective
treatment is described in Castelli, Grattton, and Kurucz 1997,
A&A 328, 841. Some colors are tabulated as well. Files
labelled coubes* are Cousins with Bessell 1990 passbands
instead of the obsolete Bessell 1979 passbands used in my
calculations.
ODFNEW = as NOVER but with newly computed ODFs with better opacities
and better abundances. (Consult Castelli; paper in preparation)
**THESE ARE THE PREFERRED MODELS**
Prefix
A = tables of temperatures-pressure relations for each model for a range
Teff and log gravity
B = Balmer line profiles for each model
F = fluxes for each model
I = intensities for each model; limbdarkening for 17 angles
All of the models from the CD-ROMs are here. Some of the models that are
weakly convective and have zero convection at the last point have a
programming error that produces a small error in the flux. This error is
detectable when computed photometry is compared to high quality observed
photometry. This error has been corrected and many of the convective models
have been recomputed. The newer models and fluxes and colors should be used
instead of those from CDROMs 13, 16, 17, and 19 which files are labelled
with an extension ending in CD such as .datCD. Strongly convective models
are not significantly affected. New CDs will be published.
All of my convective models use an overshooting approximation that moves
flux higher in the atmosphere above the top of the nominal convection zone.
Many people do not like this approximation and want a pure unphysical
mixing-length convection instead of an impure unphysical mixing-length
convection. Anyone is welcome to take the ATLAS9 programs in
[PROGRAMS.ATLAS9] and the distribution function opacities in [OPACITIES.DF*]
and to compute models with another convective treatment. Fiorella Castelli
has done that and has computed pure mixing-length grids for a number of
abundances. Those are given in directories with names suffixed with NOVER.
The user can decide for herself.
Directory logical name
[GRIDS] GRIDS
Logical name subdirectory is [grids.logical name]
GRIDM01
GRIDM02
GRIDM03
GRIDM05
GRIDM05ODFNEW
GRIDM05AODFNEW
GRIDM05NOVER
GRIDM10
GRIDM10ANOVER
GRIDM10AODFNEW
GRIDM10HE50
GRIDM10NOVER
GRIDM10ODFNEW
GRIDM15
GRIDM15NOVER
GRIDM15ODFNEW
GRIDM15ANOVER
GRIDM15AODFNEW
GRIDM20
GRIDM20NOVER
GRIDM20ODFNEW
GRIDM20ANOVER
GRIDM20AODFNEW
GRIDM25
GRIDM25NOVER
GRIDM25ODFNEW
GRIDM25ANOVER
GRIDM25AODFNEW
GRIDM30
GRIDM35
GRIDM40
GRIDM40AODFNEW
GRIDM45
GRIDM50
GRIDP00
GRIDP00AODFNEW
GRIDP00NOVER
GRIDP00ODFNEW
GRIDP01
GRIDP02
GRIDP02ODFNEW
GRIDP03
GRIDP04
GRIDP05
GRIDP05NOVER
GRIDP05ODFNEW
GRIDP05AODFNEW
GRIDP10
GRIDHBETA
GRIDHBETACASTELLI