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• W2132433618 abstract "The solar “constant” varies over time scales from minutes to years and decades. For the influence on the atmospheric energy budget time scales longer than a few days become important, for climate research information over years to decades is needed. From direct measurements of the solar “constant” during the last 10 years, by e.g. the ACRIM experiment on the Solar Maximum Mission satellite (SMM), one indeed becomes aware of substantial changes on time scales longer than days. The most important influences seem to be related to solar activity. Results from a multi-variate spectral analysis to investigate the influence of sunspots and bright magnetic elements on the total solar irradiance during 1980 and in 1984/85 show that for periods up to about 100 days, most of the power in the spectrum of the ACRIM irradiance variance is explained by the effect of the complex sunspot groups showing new activity. The correlation with old sunspots is much lower. In 1984/85, near the solar minimum, around the 27 days rotational period of the sun the greatest part of the ACRIM irradiance power spectrum is related to the enhanced UV flux, which indicates that during the solar minimum, when only a few active regions are on the sun, the main contribution to the irradiance variation arises from the active network. After eliminating the effect of sunspots and bright magnetic elements from the irradiance power spectrum, there are still peaks around 9 and 27 days. This indicates that global effects not related to the solar activity produce irradiance variations, which may be modulated by the same mechanism as that producing solar activity. The same record of the total solar irradiance shows long-term variations over the last 8 years, which are related to the activity cycle and show a difference between the maximum in 1980 and the minimum in 1986 of 0.08% with the irradiance being higher during the solar maximum. Model calculations using these directly measured values as calibration and taking into account the influence of the excess radiation from bright magnetic elements and of the dark spots are used to extend the record back to 1954. The results are also compared with measurements in the late sixties, which were obviously of much less accuracy, but can be compared at least qualitatively with the model predictions. They show also how variable the influence of the activity on the irradiance is from the cycle to cycle. La “constante” solaire varie sur des échelles de temps allant de minutes à des années et décades. Pour l'influence sur le bilan d'énergie atmosphérique, les échelles de temps supérieures à quelques jours deviennent importantes, pour la recherche climatique l'information sur des années ou décades est nécessaire. Grâce aux mesures directes de la “constante” solaire pendant les dix dernières années, par example l'expérience ACRIM sur le satellite “Solar Maximum Mission (SMM)”, on a pris conscience de changements substantiels sur des échelles de temps plus longues que le jour. Les influences les plus importantes semblent reliées à l'activité solaire. Les résultats d'une analyse spectrale multi-variée pour investiguer l'influence des taches solaires et des éléments magnétiques brillants sur l'éclairement solaire total durant 1980 et en 1984/85 montrent que pour des périodes jusqu'à environ 100 jours, la plupart de la puissance dans le spectre de variance de l'éclairement ACRIM s'explique par l'effet des groupes complexes de taches présentant une activité nouvelle. La corrélation avec les taches anciennes est plus faible. En 1984/85, prés du minimum solaire, autour de la période rotationelle de 27 jours du soleil, la plus grande partie du spectre de puissance de l'eclairement ACRIM est liée à l'augmentation du flux UV, ce qui indique que durant le minimum solaire, quand il y a seulement quelques zones actives sur le soleil, la contribution principale aux variations d'éclairement provient du réseau actif. Après élimination de l'effet des taches solaires et des éléments magnétiques brillants du spectre de l'éclairement, il y a encore des pics autour de 9 et 27 jours. Ceci indique que des effets globaux non liés à l'activité solaire produisent des variations d'éclairement, qui peuvent être modulées par le même mécanisme qui produit l'activité solaire." @default.
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• W2132433618 date "1989-10-01" @default.
• W2132433618 modified "2023-09-26" @default.
• W2132433618 title "Solar irradiance variability" @default.
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• W2132433618 doi "https://doi.org/10.1016/0169-8095(89)90027-6" @default.
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