$\begin{figure} \par\includegraphics[width=6.9cm,clip]{2043fig2.eps} \end{figure}$ Figure 2: Temperature ( top) and density ( bottom) distribution for the photosphere and chromosphere regions.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2043fig3.eps} \end{figure}$ Figure 3: Brightness temperature of the solar disk center at various frequencies from 1.4 to 405 GHz represented by symbols. The solid curve shows the result obtained from our model.
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In the text

$\begin{figure} \par\includegraphics[height=7.8cm,width=8.05cm,clip]{2043fig4.eps} \end{figure}$ Figure 4: Representation of the 2-D solar atmosphere showing the regions covered by the temperature and density matrices. In this picture, Earth direction is to the right, making disk center at $0^\circ$ and limb at the top, at $90^\circ$ .
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{2043fig5.eps} \end{figure}$ Figure 5: Center-to-limb variation of the brightness temperature at 17 GHz, obtained from the model described in the text. The solid line is the result of the convolution of the model results (crosses) with the 10'' Nobeyama synthesized beam.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2043fig6.eps} % \end{figure}$ Figure 6: The plots show the effect of the brightness temperature measured at disk center as a function of the spicule height for different values of spicules temperature and density.
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In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{2043fig8.eps} \end{figure}$ Figure 8: Brightness temperature center-to-limb variation for a single simulation using the atmospheric model with spicules.
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In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{2043fig9.eps} \end{figure}$ Figure 9: Center-to-limb brightness temperature distribution for a mean of 28 simulations using the atmospheric model with spicules (crosses). The solid line depicts the convolution of the brightness temperature with a 10'' Gaussian beam representing the NoRH spatial resolution.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2043fig10.eps} \end{figure}$ Figure 10: Brightness temperature center-to-limb variation, mean from a set of simulations using the atmospheric model with spicules of different temperatures.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2043fig11.eps} % \end{figure}$ Figure 11: Brightness temperature center-to-limb variation, mean from a set of simulations using the atmospheric model with spicules of different densities.
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In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{2043fig13.eps} \end{figure}$ Figure 13: Comparison between the observational profile at the equator (gray) and the mean of the simulations (black).
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In the text

$\begin{figure} \par\includegraphics[width=6.75cm,clip]{2043fig1.eps} \end{figure}$	Figure 1: NoRH map of the Sun at 17 GHz, with the brightness close to the limb enhanced.
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$\begin{figure} \par\includegraphics[width=6.9cm,clip]{2043fig2.eps} \end{figure}$	Figure 2: Temperature ( top) and density ( bottom) distribution for the photosphere and chromosphere regions.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2043fig3.eps} \end{figure}$	Figure 3: Brightness temperature of the solar disk center at various frequencies from 1.4 to 405 GHz represented by symbols. The solid curve shows the result obtained from our model.
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$\begin{figure} \par\includegraphics[height=7.8cm,width=8.05cm,clip]{2043fig4.eps} \end{figure}$	Figure 4: Representation of the 2-D solar atmosphere showing the regions covered by the temperature and density matrices. In this picture, Earth direction is to the right, making disk center at $0^\circ$ and limb at the top, at $90^\circ$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{2043fig5.eps} \end{figure}$	Figure 5: Center-to-limb variation of the brightness temperature at 17 GHz, obtained from the model described in the text. The solid line is the result of the convolution of the model results (crosses) with the 10'' Nobeyama synthesized beam.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2043fig6.eps} % \end{figure}$	Figure 6: The plots show the effect of the brightness temperature measured at disk center as a function of the spicule height for different values of spicules temperature and density.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{2043fig7.eps} \end{figure}$	Figure 7: Distribution of spicules over the solar limb.
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$\begin{figure} \par\includegraphics[width=7.25cm,clip]{2043fig8.eps} \end{figure}$	Figure 8: Brightness temperature center-to-limb variation for a single simulation using the atmospheric model with spicules.
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$\begin{figure} \par\includegraphics[width=7.25cm,clip]{2043fig9.eps} \end{figure}$	Figure 9: Center-to-limb brightness temperature distribution for a mean of 28 simulations using the atmospheric model with spicules (crosses). The solid line depicts the convolution of the brightness temperature with a 10'' Gaussian beam representing the NoRH spatial resolution.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2043fig10.eps} \end{figure}$	Figure 10: Brightness temperature center-to-limb variation, mean from a set of simulations using the atmospheric model with spicules of different temperatures.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2043fig11.eps} % \end{figure}$	Figure 11: Brightness temperature center-to-limb variation, mean from a set of simulations using the atmospheric model with spicules of different densities.
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$\begin{figure} \par\includegraphics[width=7.4cm,clip]{2043fig12.eps} \end{figure}$	Figure 12: Solar radius dependence on average spicule height, h.
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$\begin{figure} \par\includegraphics[width=7.25cm,clip]{2043fig13.eps} \end{figure}$	Figure 13: Comparison between the observational profile at the equator (gray) and the mean of the simulations (black).
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