Issue 
A&A
Volume 552, April 2013



Article Number  A114  
Number of page(s)  8  
Section  The Sun  
DOI  https://doi.org/10.1051/00046361/201220512  
Published online  11 April 2013 
Online material
Appendix A: Model description
The annual solar Strömgren (b + y)/2 flux values F(t) can be decomposed into the longterm F^{LT}(t) and cyclic F^{11}(t) components (see, e.g. Tapping et al. 2007) (A.1)While cyclic component F^{11}(t) varies on the 11year time scale and controls the activity cycle, the longterm component F^{LT}(t) varies on secular time scales and leads to a changeable level of the flux during the solar activity minima.
Most of the stars in the Lockwood et al. (2007) dataset are observed over an approximately 20year period. Therefore, to compare stellar and solar variabilities we will introduce the rms_{20} value. For any given year t, it is the rms variability of the dataset which consists of twenty annual flux values (from year t−9, till year t + 10).
The total variability of the solar flux can be calculated as the geometrical sum of the longterm and cyclic variabilities (A.2)We introduce parameter V_{11} as rms variability of the annual (b + y)/2 flux values for the 1976–1996 period (solar cycles 21 and 22). The Krivova et al. (2010), Shapiro et al. (2011), and Lean et al. (2005) reconstructions show the value of V_{11} parameter equals 0.00019 mag, 0.00018 mag, and 0.000032 mag, respectively.
To calculate the cyclic component backwards in time, we assume that its amplitude is proportional to the longterm solar activity φ(t). The latter can be reconstructed over the millennia from the cosmogenic isotope data, which gives a 22year running mean of the modulation potential (Steinhilber et al. 2008; Herbst et al. 2010). Thus, the cyclic rms variability for any given year t can be calculated as (A.3)where φ(t) is the modulation potential and φ(t_{0}) is the mean value of the modulation potential for the 1976–1996 period. The modulation potential is deduced from the composite of the neutron monitor data (Usoskin et al. 2005) and ^{10}Be data (McCracken et al. 2004; Vonmoos et al. 2006). It is normalised to the Castagnoli & Lal (1980) local interstellar spectra. The homogenisation procedure is discussed in Shapiro et al. (2011) and Thuillier et al. (2012). The average uncertainty of the modulation potential changes is ~80 MeV (Vonmoos et al. 2006) and does not have a significant contribution to the temporary mean of the solar variability.
To calculate the rms_{20}(F^{LT}(t)) contribution we introduce parameter V_{LT} as a relative change of F^{LT} between the present and the Maunder minimum. The changes of the solar flux between three recent solar minima are within the uncertainties of the reconstructions and measurements of the solar irradiance (see review by Ermolli et al. 2012), so the F^{LT} component can be approximated by a constant for the last solar cycles. Therefore, for simplicity we define V_{LT} as the relative change of the (b + y)/2 flux between the 1996 and the Maunder minima.
We assume that the longterm changes of the solar irradiance are proportional to the changes of the solar activity φ(t) (A.4)where t_{0} refers to our reference period (1976–1996 average) and t_{M} refers to the Maunder minimum.
Substituting F^{LT}(t_{M}) − F^{LT}(t_{0}) = V_{LT} F^{LT}(t_{0}), one can connect the relative changes of the solar flux and activity (A.5)Equation (A.5) links rms_{20}(F^{LT}(t)) and rms_{20}(φ(t)) via the parameter V_{LT}. In combination with Eqs. (A.2) and (A.3) it allows one to reconstruct the solar variability backwards in time as a function of V_{11} and V_{LT} parameters.
The approach, presented above is based on three assumptions:

1.
The amplitude of the activity cycle is proportional to thelongterm (i.e. cycleaveraged) solar activity.

2.
The longterm changes of the solar irradiance are proportional to the longterm changes of the solar activity.

3.
The longterm solar activity can be reconstructed from the cosmogenic isotope data.
Let us note that these assumption are either employed or fulfilled because of the physical reasons in most of the available reconstructions, independently from the proposed mechanism for the secular changes.
To estimate the accuracy of our approach we consider three different reconstructions of the solar irradiance to the past: Krivova et al. (2010) (V_{LT} = 0.044%, V_{11} = 0.000019 mag), Shapiro et al. (2011) with removed longterm trend (V_{LT} = 0%, V_{11} = 0.000018 mag), and the original Shapiro et al. (2011) reconstruction (V_{LT} = 0.38%, V_{11} = 0.000018 mag). They yield 0.0001 mag, 0.00009 mag, and 0.00036 mag for the mean solar rms_{20} variability over the 1620–1995 period. The same values calculated with the set of Eqs. (A.2)–(A.5) are 0.00013 mag, 0.00012 mag, and 0.00035 mag. One can see that our approach slightly overestimates the first two numbers. The reason for this is that to allow a homogeneous reconstruction over the millennia we use the solar modulation potential to scale the cyclic variability (see Eq. (A.3)) instead of the sunspot number. The annual sunspot number is very close to zero during the Maunder minimum period, so the reconstructions predict the cessation of the cyclic variations (see Fig. 2). At the same time the modulation potential and consequently the cyclic variability in our approach did not go to zero during the Maunder minimum (McCracken et al. 2004). Such deviations are comparable to the uncertainties of the reconstructions and are not essential for our conclusions.
Fig. B.1
Left panel: the dependency of the V_{LT} parameter on the solar variability, retrieved from the stellar data. The shaded area indicates the uncertainty (2σ) due to the limited number of stars. The V_{11} parameter is set to 0.00044 mag. The dashed line corresponds to the expected mean solar variability rms_{20} = 0.00082. The projection onto V_{LT}axis yields the 95% interval for expected longterm variability of the Sun: 0.43% < V_{LT} < 0.76%. Right panel: the same as the left panel, but the contour calculated with V_{11} = 0.0002 mag is added. The four dashed lines correspond to four values of expected mean solar variability rms_{20}: 0.00097 mag (no chromospheric secular changes, regression with solid line from Fig. 1), 0.00082 mag (strong chromospheric secular changes, regression with solid line), 0.00065 mag (no chromospheric secular changes, regression with dashed line), 0.00053 mag (strong chromospheric secular changes, regression with dashed line). The projection onto the V_{LT}axis yields the interval 0.17% < V_{LT} < 1.2%. 

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Fig. B.2
Upper panel: rms_{20} back to 400 BC, adopting V_{LT} = 0.001 (lower curve) and V_{LT} = 0.005 (upper curve). V_{11} is set to 0.0002 mag. Lower panel: modulation potential back to 400 BC. The interval in the upperright corner denotes the satellite era of continuous solar irradiance measurements. 

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The calculation of the Ca II H and K lines, which are used to determine the solar chromospheric activity, made even more complicated by the effect of the nonlocal thermodynamical equilibrium (Ermolli et al. 2010). So the mean solar chromospheric activity cannot be directly deduced from the available reconstructions of the solar irradiance over the millennia. Instead we will linearly scale it with the longterm solar activity (A.6)where is the present value of the mean solar chromospheric activity (, see Lockwood et al. 2007) and is the value of the mean chromospheric activity corresponding to φ = 0.
In Fig. 3 we consider two extreme scenarios (see Sect. 3), one without the secular component in the solar chromospheric activity, and another with a strong secular component. Without the secular component the changes of the mean solar chromospheric activity are only caused by the variable amplitude of the solar activity cycle and the value corresponds to the present value of the solar activity at minimum conditions (; see Judge & Saar 2007). To describe the case of a strong secular component in the chromospheric activity we put the value equals to the boundary value from Saar (2006) ().
Appendix B: Possible constraints on the historical solar variability
The amplitude of the secular solar photometric variability can be constrained by demanding the temporal mean solar variability be in agreement with the variability, indicated by the stellar data. The latter depends on the version of the variability versus activity regression and the scenario of the chromospheric activity behaviour. To investigatedifferent cases in Fig. B.1 we plot the longterm solar variability V_{LT} as a function of the mean solar variability (rms_{20}) given by the stellar data, for two values of the 11year variability V_{11}. The inclination effect was calculated according to Knaack et al. (2001).
Let us note, however, that the positions of the Sunlike stars in Fig. 3 are also not necessarily fixed in time. This can affect the coefficients of the regression line and accordingly the estimated variability of the Sun. For example it is possible that, by coincidence, most of the stars among the twentyone used for our analysis represent the periods of the relatively low (or high) variability. This will lead to the shifted position of the regression line and consequently to the deviations in the V_{lt} parameter determined using this limited selection of stars.
If the behaviour of the stellar variabilities after the regression to the solar level of the chromospheric activity is identical to the solar variability, i.e. the solar and regressed stellar variabilities can be parameterised employing the approach described in Sect. 3 and Appendix A, then the resulting uncertainty can be found by performing the Monte Carlo simulation. To do this we considered a large number of sets consisting of 21 stars. Every star in these sets represents the Sun at some random twentyyear interval period (chosen from the full 9000year dataset) and with a random angle between the stellar rotation axes and the direction to the observer. The rms_{20} variability of these stars is calculated, employing the approach described in Sect. 3 and Appendix A and the Knaack et al. (2001) dependency of the 11year variability on the angle between the solar rotation axes and the direction to the observer. For every set we calculated the mean rms_{20} variability of the stars in the set, so for every pair of V_{LT} and V_{11} parameters we have a distribution of mean rms_{20} variabilities. This allows us to calculate the range of V_{LT} and V_{11} parameters which can lead to the present value of the linear coefficients of the activity versus variability regression line. In Fig. B.1 we mark the resulting 2σ uncertainty in V_{LT} parameter with a shaded area.
The mean solar index in the case of the strong secular component in chromospheric activity is − 4.96 (see Fig. 3). Using the solid blue line in Fig. 1 one can find that this index corresponds to the 8.2 × 10^{4} rms variability. This value is inserted in the left panel of Fig. B.1 and one can see that it yields V_{LT} = (0.43%−0.76%).
In the right panel of Fig. B.1 we also plotted the contour with V_{11} = 0.0002 mag and indicated four different values of the expected solar variability, corresponding to different treatments of the chromospheric secular changes and two regressions from Fig. 1. One can see that the minimum value of V_{LT} equals 0.17%.
The parameter V_{LT} characterises the longterm variability as it is observed in the Strömgren b and y filters. Its connection with the variability at another spectral domain (or TSI) depends on the mechanism of the secular changes. For example a V_{LT} equal to 0.17% leads to a 2.7 W/m^{2} TSI change between the Maunder and the last solar minima, adopting the model of Shapiro et al. (2011), and to 1.9 W/m^{2}, assuming that it is caused by the variations of the solar effective temperature.
© ESO, 2013
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