We use the model atmosphere code PHOENIX (version 10.8). The original
versions of PHOENIX were developed for the modeling of novae and
supernovae ejecta described by ,
and is dotted of a detailed radiative transfer that
allows for spherical symmetry. Its more recent application to cool
dwarfs is described in detail by , and has served
to generate grids of stellar model atmospheres which successfully
described low mass stars in globular clusters
and the galactic disk main sequence
. These former model grids are known to the stellar
community as the 1995 Extended and the 1996-1999 NextGen models, and
allowed a preliminary incursion into the regime of evolved brown
dwarfs down to T
K (Extended models) and to 900K
. These models successfully predicted the general
spectroscopic properties of evolved brown dwarfs prior to the
discovery of Gliese 229B, which then helped confirm its very cool
brown dwarf nature . Yet the lack, in
these essentially stellar models, of dust condensation in the chemical
equilibrium made them inadequate to model in detail such cool objects.
The addition to PHOENIX of the treatment of condensation in the chemical
equilibrium, and of dust clouds, as described in Sections
and 3, was completed in 1996 , and served to compute
M dwarfs and brown dwarfs model atmospheres, synthetic spectra and
broadband colors for specific analysis and
interior models . In this paper we present the final
version of these models in two limiting cases: (1) ``AMES-Dusty''
which include both the dust formation in the chemical equilibrium and
opacities, and; (2) ``AMES-Cond'' which include the effects of
condensation in the chemical equilibrium but ignores the effects of
dust opacities altogether. This latter case is computed to explore
the case where dust grains have formed, but have disappeared
completely (eg by sedimentation i.e. settling below the photosphere).
These two model sets also distinguish themselves from the standard
NextGen models by the use of the NASA AMES H2O and TiO line lists
while the NextGen models were computed using the
line list. This choice is motivated by the
incompleteness of the 1994 lists to high gas temperatures (T
gas >
2000K) as discussed in .
For the purpose of this analysis, we use the radiative transfer in
plane-parallel mode. The convective mixing is treated according to
the Mixing Length Technique (MLT). We consider pressure-dependent
line-by-line opacity sampling treatment for both atomic and molecular
lines in all models. We do not pre-tabulate or re-manipulate
the opacities in any way: PHOENIX includes typically
molecular and atomic transitions which are re-selected at
each model iteration and each atmospheric depth point from our data
base described above. The lines are selected from three
representative layers of the atmosphere at each model iteration to
ensure consistency of the calculation. Van der Waals pressure
broadening of the atomic and molecular lines is applied as described
by . We neglect the effects of convective motion on
line formation since the velocities of the convection cells are too
small to be detected in low-resolution spectra and will have a
negligible influence on the transfer of line radiation.
A trial atmospheric profile is applied, the equations of hydrostatic
and radiative transfer are solved, and the solution is tested until
convergence is reached. The model is considered converged when the
energy is conserved within a tenth of a percent from layer to layer.
At each of the model iterations, a spectrum with typically over 30,000
points is generated which samples the bolometric flux from 0.001 to
500 m with a step of 2Å in the region where most of the flux
is emitted (i.e. 0.1 to 10
m). The final spectrum must
generally be degraded to the instrumental resolution before
being compared to low-resolution observations of stars and brown
dwarfs. The model atmospheres are characterized by the following
parameters: (i) the surface gravity,
,
(ii) the effective
temperature,
,
(iii) the mixing length to scale height
ratio,
,
here taken to be unity, (iv) the micro-turbulent
velocity
,
here set to
,
and (v) the element abundances
taken from .
For this paper we have calculated a uniform grid of AMES-Cond models
ranging from
to 100K in 100K steps, and with gravities
ranging from
to 6.0 in steps of 0.5 dex at solar
metallicity. The AMES-Dusty grid was calculated from
to 1400K in steps of 100K, with gravity ranging from
to
6.0 in steps of 0.5 dex. All models were fully converged.
Although PHOENIX can treat the effects of external radiation fields on the model atmosphere and the synthetic spectrum , we assume here a negligible external radiation field for simplicity. It is clear, however, that UV radiation impinging on the brown dwarf, from a hotter companion, will change the structure of the atmosphere and the corresponding spectra. We are investigating these effects in a separate publication .
.