All Figures

Figure 1: The pooled variance of the relative variations of the TSI and SSIs as a function of the time interval  chosen to bin the data. The different symbols refer to the different spectral passbands as follows: open diamonds - 402 nm; asterisks - 500 nm; open squares - 862 nm; filled circles - total solar irradiance. The main ranges of variation of the pooled variance are indicated with A, B, C, D and E and are separated by vertical dotted lines at 2, 8, 32 and 56 days, respectively.

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In the text

	Figure 2: The sunspot contrasts adopted in our model ( ) versus the temperature difference of the sunspots with respect to the unperturbed photosphere  . Different linestyles refer to different passbands: TSI - solid; 402 nm - dotted; 500 nm - dashed; 862 nm - dash-dotted.
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In the text

	Figure 3: The facular contrasts adopted in our model ( ) versus the temperature excess of the faculae with respect to the unperturbed photosphere  . Different linestyles refer to different passbands: TSI - solid; 402 nm - dotted; 500 nm - dashed; 862 nm - dash-dotted.
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In the text

	Figure 4: The isocontour plots of the ratio-of-variance statistics   versus sunspot temperature deficit  and facular temperature excess  for the data subset ranging from 16 July 1996 to 17 August 1996, close to the minimum of solar activity cycle 23.
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In the text

	Figure 5: The of the individually fitted data subsets of length 14 days versus time computed according to Eq. (2). The time is indicated in days counting from 1st January 1996 on the lower scale and in years on the upper scale.
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In the text

Figure 6: Two subsets of the TSI and SSI time series during the minimum of solar cycle 23 (open diamonds) with their respective best fits (solid lines) are plotted in panels a), c), e) and  g) for the labelled passbands in the left and the right columns, respectively. The model is usually embedded into the data sequence except when data gaps are present. The residuals are plotted in the corresponding lower panels b), d), f) and  h), respectively. The time is indicated in days from 1st January 1996 on the lower scale and in years on the upper scale. The data subsets range from 13 July 1996 to 11 September 1996 on the left panels, including the intervals previously analysed by Eker et al. (2003) and Fligge et al. (2000, Fig. 6), and from 5 November 1996 to 4 January 1997 on the right panels, previously analysed by Fligge et al. (2000, Fig. 7), respectively.

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In the text

	Figure 7: The same as Fig. 6 for two data subsets close to the maximum of solar cycle 23, ranging from 29 January 2000 to 29 March 2000 in the left panels, and from 29 March 2000 to 28 May 2000 in the right panels, respectively. These time series were previously modelled by Krivova et al. (2003, Fig. 3 right panels).
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In the text

Figure 8: From the upper to the bottom left panels: the gain spectrum , the phase spectrum and the square of the modulus of the coherency |w|2 versus frequency for our model time series versus the corresponding observed time series during the interval ranging from 1996.25 to 1997.75. Different linestyles mark the four passbands: solid - TSI; dotted - 402 nm; dashed - 500 nm; dash-dotted - 862 nm. From the upper to the bottom right panels: the same as the left panels for the interval ranging from 1999.5 to 2001.0.

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In the text