In this paper, we account for the dust opacity only in the limiting case of the AMES-Dusty models where gravitational settling is neglected and which are relevant for the analysis of hot red dwarfs. In these models, cloud layers build up automatically following the condensation equilibrium which determines the atmospheric layers occupied by the grains. The study of the jovian planets suggests that cloud layers are not generally distributed homogeneously over the atmospheric surface. But if the nucleation process of dust grains is favored by a combination of high gas densities and low gas temperatures, hotter red dwarfs could be expected to retain more easily smaller grains in their photosphere, and have them more uniformly distributed over the stellar surface. In this work, we account for the average effect of the presence of clouds on the model structures and emitted spectra. We therefore assume a plane-parallel symmetry, i.e. an homogeneous distribution of clouds across the surface of the brown dwarfs. The spectral distribution of a brown dwarf with a more complex ring pattern of clouds familiar to jovian planets could, in the end, be reconstructed from a mosaic of the present models until a full three dimensional calculation becomes possible.
Early attempts to compute the opacities of grains were made by
and . More detailed calculations,
including the effects of chemical equilibrium calculations and grain
size distributions were reported by and
. have described the computation of the
opacity of grains with the inclusion of equilibrium condensation
abundances, the effects of the distribution of grain sizes, and the
effect of grain shape through the Continuous Distribution of Ellipsoid
(CDE) model of . These calculations included
the absorption and scattering due to magnesium silicates, iron,
carbon, and silicon carbide grains for a wide range of chemical
compositions down to 700 K. We have explored the CDE method employed
by Alexander & Ferguson, but have retained a purely spherical shape
of the grains in the present study for simplicity. Another difference
with Alexander & Ferguson is that, instead of approximating the
number density of grains indirectly, these quantities are now provided
by our chemical equilibrium as described in Section . 26 new
condensates have been added to the original list of Fe, C, SiC and
magnesium silicates, for a total of 30 among which are MgSiO3,
Mg2SiO4, Al2O3 and MgAl2O7, using polarizability
constants from laboratory studies by ,
, , and .
Figure
and 2 suggest that the calcium
silicates can also play an important role in the opacity of brown
dwarf atmospheres. In fact, complex calcium silicates (here
Ca2Al2SiO7, Ca2MgSi2O7, and CaMgSi2O6) are
amoung the most abundant species in the layers where these grains are
present. Since, for the latter two species, no data were available to
construct their opacity profiles, we have simulated their opacity
using the profile of Ca2Al2SiO7. We includes in general,
more accurate number densities, and better and more complete
cross-sections of dust grains than included in . Updated
Rosseland and Planck opacities computed with these updated opacities
will be published in more details separately .
The opacity profiles of these grains are shown in Figure .
Most spectral distributions seen in this plot are pure absorption
profiles. Scattering contributes only at UV to optical wavelengths
for the grain sizes adopted. Corundum, enstatite, forsterite,
hematite, magnetite, and Ca2Al2SiO7 have absorption
cross-sections exceeding those of water vapor. In a brown dwarf
atmosphere, however, water is at least two orders of magnitudes more
abundant then most of these grain species, so that water vapor remains
the leading opacity source between 1 and 8
,
and beyond 20
m. In other words, grains do not contribute significantly to the
opacities in the near-infrared where water bands still dominate the
brown dwarf spectra from J to K (1.0 to 3
m). We have
demonstrated in Section 2 that grain species have
concentrations similar to those of TiO, VO and most other optical
absorbers. The impact of the grain opacities is, therefore, to
enhance and gradually replace the optical opacities as these gas phase
species disappear via condensation.
The extinction caused by grains in a stellar atmosphere also depends
on the rate of grain formation and the resulting size distribution.
For all grains included we have assumed, as in Alexander & Ferguson,
an interstellar size distribution of the grains with diameters ranging
from 0.00625 to 0.24 m. For comparison, and
assumed grains with a fixed diameter of 0.1
m in
their model atmosphere calculations. Although those choices are
purely arbitrary, the consequences are minimal since the grain
diameter cancels out in the opacity calculations as long as: (1)
abundance conservation is assumed i.e. larger grains must lock more
particles, reducing the number of grains per gram of stellar plasma,
and, (2) that the cross-sections behave in the Rayleigh limit, i.e.
the wavelength is larger than the size of the grains. Our tests,
shown in Figure
, confirm that this is the case for 1 to 10
m-size grains, but they also indicate that the scattering
increases rapidly for sizes larger than 10
m, i.e. when the
Rayleigh limit beaks down over the wavelengths carrying flux in these
objects. But even is the opacities are sensitive to the grain sizes
beyond the Rayleigh regime, the enormous scattering effects seen for
100
m grains in Figure 4 seems to exclude the presence
of such grains in brown dwarfs. We therefore believe that such large
grains tend rapidly to become larger by coagulation to be eliminated
by sedimentation in these high-gravity atmospheres. An accurate
answer to this question can only come from time-dependent grain growth
calculations incorporating the effects of sedimentation, diffusion,
coagulation and coalescence for the conditions prevailing in brown
dwarfs atmospheres. See for a detailed description of
the dust opacities used in the present models.
for a detailed description of the dust opacities used in the present models.