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Figure 2: a)Measured (symbols) and modelled (standard model; solid line) totalmagnetic flux between 1974 and 2002.Each data point is an integral over a synoptic chart for one Carringtonrotation.Different symbols are used for different data sets: filled circles represent theWSO data, open triangles the KP NSO data and open squares the MWO measurements(cf. Wenzler et al. 2006; Arge et al. 2002).For the modelled flux the value is given (seeSect. 2.3). b) and c) Reconstructed magnetic flux in AR (grey solid curve),ER (dotted), as well as the open (dot-dashed) and total (black solid)flux since 1974 and 1700, respectively.Open with DEXTER Figure 3:Evolution of the open flux since 1700: calculated with the standardmodel (solid curve) and reconstructed by Lockwood et al. (1999)from the geomagnetic aa-index (dashed).Open with DEXTER Figure 4:Modelled (standard model; dots) and observed (PMOD composite,grey solid line) variations of the total solar irradiance in cycles 21-23. a) Daily values; b) 3-month runnning means; c) thedifference between the model and the data (each dot represents a dailyvalue, the bigger filled circles 30 day averages).Open with DEXTER Figure 5: a) Reconstructed TSI since 1700 for the standard model. b) 11-yr running mean of the reconstructed TSI for the standard(solid line),"antiphase (2)'' (dashed) and "constant (2)'' (dotted) models.Open with DEXTERNext, we convert the network, ,and facular, ,magnetic fluxes intocorresponding filling factors, and .For this, we use the same conversion scheme as in previous applications ofthe SATIRE models(Wenzler et al. 2005; Krivova et al. 2003; Wenzler et al. 2006,2004):and are proportional to and ,respectively, until a saturation limit is reached where(see previous papers for more details).Above they remain constant.is a free parameter of the SATIRE models, which depends onthe resolution and the noise level of the employed magnetic field maps.The smaller the fraction of the true magnetic flux visible in themagnetograms, the smaller the needs to be.In order to reproduce solar irradiance variations in cycle 23 on the basisof MDI magnetograms, Krivova et al. (2003) found G (no distinction was made between faculae and the network).For a reconstruction of solar irradiance in cycles 21-23 based onNational Solar Observatory Kitt Peak (NSO KP) data,Wenzler et al. (2005,2006) found -320 G to be more adequate.The larger is consistent with the fact that KP magnetogramshave a lower noise level than those from the MDI.Since magnetic field strengths in faculae are higher than the noise level ofeither of these 2 sets of images, we do not expect a considerable differencein the value and used the value of 300 G as our primaryestimate.In some extreme cases (see Sects. 3.2 and 3.3),however, we allowed to vary.Faculae mainly appear in the so-called activity belts (i.e. at latitutesbetween approximately (5-15) and (40-45) degrees), and theirdistribution therefore peaks at -values above 0.9 (see, e.g., Fig. 11bin Wenzler et al. 2006).However, faculae become fainter when they cross the disc centre(e.g., Ortiz et al. 2002).By assuming a homogeneous distribution of faculae over the solarsurface, we overestimate their contribution to the brightening of theSun, since the ratio of low-to large-area is smaller foractivity belts than for the whole disc.We take this into account by weighting facular contributions, with weightsproportional to the fraction of the solar disc occupied by each-bin within activity belts and 0 outside of these.The weakest network elements are lost within the noiselevel and, since they are often present as mixed polarity features, they arealso lost due to apparent cancellation of polarities caused by insufficientspatial resolution of the MDI or KP magnetograms(Krivova & Solanki 2004).Consequently, in case of noise-free high resolution data, their saturationflux could lie significantly higher than 300 G deduced from MDI and KPmagnetograms.In order to estimate for such ideal "noise-free'' data,we utilised MDI magnetograms with different noise levels to recontsruct solarirradiance on 70 days between the minimum of cycle 23 in 1996 andits maximum in 2000 following Krivova et al. (2003).For this, we consecutively averaged MDI magnetograms over 5, 20 or 59min (which reduced the noise level down to approximately8.9 G, 4.5 G and 2.6 G, respectively) and employed these together with theoriginal 1-min data (having the noise level of about 20 G) forthe reconstruction.In each case, the value of was found from a comparison withthe irradiance variations measured by the VIRGO instrument on SoHO(Fröhlich & Finsterle 2001).The dependence of the on the noise level of the employedmagnetograms is shown in Fig. 1.An extrapolation to the 0-noise level (see Fig. 1) suggestsa value of of around 500 G, which we use in this work.The magnetic fluxes reconstruted with the model described inSect. 2.1 are integrals over the solar disc.Thus the filling factors obtained using and are averages over thesolar disc: 2ff7e9595c
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