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Figure:
Temperature structures for solar abundance models with
, , and for varying gravities (as indicated).
is the optical
depth in the continuum (bf and ff processes) at a wavelength of m.

Figure:
Radial extensions
for solar abundance models with
, , and (as indicated).

Figure:
Comparison between solar abundance giant models
calculated using spherical geometry and radiative transfer (full curves) and
plane parallel geometry and radiative transfer(dotted curves) in the
blue/optical spectral region. The resolution of the spectra has been reduced to
.

Figure:
Relative flux change between spherical and plane parallel
model calculations. The yaxis shows (f_{p}f_{s})/f_{s}, where f_{p} is the flux of
the plane parallel model and f_{s} is the flux calculated for the spherical model.
The resolution of the spectra was reduced to .

Figure:
Relative flux change between spherical and plane parallel
model calculations. The yaxis shows (f_{p}f_{s})/f_{s}, where f_{p} is the flux of
the plane parallel model and f_{s} is the flux calculated for the spherical model.
The resolution of the spectra is .

Figure:
Relative flux change between spherical and plane parallel
model calculations. The yaxis shows (f_{p}f_{s})/f_{s}, where f_{p} is the flux of
the plane parallel model and f_{s} is the flux calculated for the spherical model.
The resolution of the spectra was reduced to .

Figure:
Relative flux change between spherical and plane parallel
model calculations. The yaxis shows (f_{p}f_{s})/f_{s}, where f_{p} is the flux of
the plane parallel model and f_{s} is the flux calculated for the spherical model.
The resolution of the spectra is .

Figure:
Temperature structures for spherical (full curves)
and plane parallel (dotted lines) model calculations. is the optical
depth in the continuum (bf and ff processes) at a wavelength of m.

Figure:
Sensitivity of the synthetic spectra to gravity
changes for solar abundance models with , , and (as indicated). The resolution of the spectra has been reduced to .

Figure:
Sensitivity of the synthetic spectra to metallicity
changes for models with , , and
(as indicated) and . For the model the metallicities
and are shown whereas for the hotter two models the
metallicities shown are and .The resolution of the spectra has been reduced to .

Figure:
Synthetic spectra at resolution
for models with , , solar abundances, and
stellar masses of and .

Figure:
Overview over selected departure coefficients
for a NLTE model with , , and solar abundances.

Figure:
Overview over selected departure coefficients
for a NLTE model with , , and solar abundances.

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Up: The NextGen Model Atmosphere
Previous: References
Peter H. Hauschildt
7/14/1999