Figures

 

Figure:   Temperature structures for solar abundance models with $\hbox{$\,T_{\rm eff}$}=5600\,{\rm K}$, $4200\,{\rm K}$, and $3000\,{\rm K}$ for varying gravities (as indicated). $\ifmmode{\tau_{\rm std}}\else\hbox{$\tau_{\rm std}$}\fi$ is the optical depth in the continuum (b-f and f-f processes) at a wavelength of $1.2\,\mu$m.

 

Figure:   Radial extensions $R_{\rm out}/R_{\rm in}$ for solar abundance models with $\hbox{$\,T_{\rm eff}$}=5600\,{\rm K}$, $4200\,{\rm K}$, and $3000\,{\rm K}$ (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 $20\hbox{\AA}$.

 

Figure:   Relative flux change between spherical and plane parallel model calculations. The y-axis 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 $20\hbox{\AA}$.

 

Figure:   Relative flux change between spherical and plane parallel model calculations. The y-axis 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 $2\hbox{\AA}$.

 

Figure:   Relative flux change between spherical and plane parallel model calculations. The y-axis 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 $20\hbox{\AA}$.

 

Figure:   Relative flux change between spherical and plane parallel model calculations. The y-axis 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 $2\hbox{\AA}$.

 

Figure:   Temperature structures for spherical (full curves) and plane parallel (dotted lines) model calculations. $\ifmmode{\tau_{\rm std}}\else\hbox{$\tau_{\rm std}$}\fi$ is the optical depth in the continuum (b-f and f-f processes) at a wavelength of $1.2\,\mu$m.

 

Figure:   Sensitivity of the synthetic spectra to gravity changes for solar abundance models with $\hbox{$\,T_{\rm eff}$}=5600\,{\rm K}$, $4200\,{\rm K}$, and $3000\,{\rm K}$(as indicated). The resolution of the spectra has been reduced to $20\hbox{\AA}$.

 

Figure:   Sensitivity of the synthetic spectra to metallicity changes for models with $\hbox{$\,T_{\rm eff}$}=5600\,{\rm K}$, $4200\,{\rm K}$, and $3200\,{\rm K}$ (as indicated) and $\log(g)=0.0$. For the $\hbox{$\,T_{\rm eff}$}=3200\,{\rm K}$ model the metallicities $[{\rm M/H}]=0.0$ and $[{\rm M/H}]=-0.3$ are shown whereas for the hotter two models the metallicities shown are $[{\rm M/H}]=0.0$ and $[{\rm M/H}]=-0.7$.The resolution of the spectra has been reduced to $20\hbox{\AA}$.

 

Figure:   Synthetic spectra at $20\hbox{\AA}$ resolution for models with $\hbox{$\,T_{\rm eff}$}=3600\,{\rm K}$, $\log(g)=0.0$, solar abundances, and stellar masses of $7.5\hbox{$\,$M$_\odot$}$ and $2.5\hbox{$\,$M$_\odot$}$.

 

Figure:   Overview over selected departure coefficients for a NLTE model with $\hbox{$\,T_{\rm eff}$}=4000\,{\rm K}$, $\log(g)=0.0$, and solar abundances.

 

Figure:   Overview over selected departure coefficients for a NLTE model with $\hbox{$\,T_{\rm eff}$}=5600\,{\rm K}$, $\log(g)=0.0$, and solar abundances.