Reconstruction of total solar irradiance 1974–2009

Ball, William T.; Unruh, Y. C.; Krivova, N. A.; Solanki, S. K.; Wenzler, T.; Mortlock, D.; Jaffe, A. H.

doi:10.1051/0004-6361/201118702

Cited by 108 publications

(193 citation statements)

References 46 publications

(129 reference statements)

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“…The latter result is also evident in the upgraded SATIRE model (Ball et al 2012). Thus, if ERB requires some correction during the ACRIM Gap, our results suggest that Fröhlich overestimated those corrections by at least a factor of two due to the fact that at least one of the two hypotheses (the ERB glitch in Sep/29/1989 or the ERB drift from Oct/1989 to 1992) are not confirmed by our cross-analysis.…”

Section: Resultscontrasting

confidence: 56%

ACRIM total solar irradiance satellite composite validation versus TSI proxy models

Scafetta

Willson²

2014

Astrophys Space Sci

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The satellite total solar irradiance (TSI) database provides a valuable record for investigating models of solar variation used to interpret climate changes. The 35-year ACRIM total solar irradiance (TSI) satellite composite time series has been updated using corrections to ACRIMSAT/ACRIM3 results for scattering and diffraction derived from recent testing at the Laboratory for Atmospheric and Space Physics/Total solar irradiance Radiometer Facility (LASP/TRF). The corrections lower the ACRIM3 scale by about 5000 ppm, in close agreement with the scale of SORCE/TIM results (solar constant ≈ 1361 W/m 2 ) but the relative variations and trends are not changed. Differences between the ACRIM and PMOD TSI composites, particularly the decadal trending during solar cycles 21-22, are tested against a set of solar proxy models, including analysis of Nimbus7/ERB and ERBS/ERBE results available to bridge the ACRIM Gap (1989Gap ( -1992. Our findings confirm the following ACRIM TSI composite features: (1) The validity of the TSI peak in the originally published ERB results in early 1979 during solar cycle 21; (2) The correctness of originally published ACRIM1 results during the SMM spin mode (1981)(1982)(1983)(1984); (3) The upward trend of originally published ERB results during the ACRIM Gap; (4) The occurrence of a significant upward TSI trend between the minima of solar cycles 21 and 22 and (5) a decreasing trend during solar cycles 22 -23. Our findings do not support the following PMOD TSI composite features: (1) The downward corrections to originally published ERB and ACRIM1 results during solar cycle 21; (2) A step function sensitivity change in ERB results at the end-of-September 1989; (3) the validity of ERBE's downward trend during the ACRIM Gap or (4) the use of ERBE results to bridge the ACRIM Gap. Our analysis provides a first order validation of the ACRIM TSI composite approach and its 0.037%/decade upward trend during solar cycles 21-22. The implications of increasing TSI during the global warming of the last two decades of the 20th century are that solar forcing of climate change may be a significantly larger factor than represented in the CMIP5 general circulation climate models.Cite: Scafetta, N., and R. C. Willson, 2014. ACRIM total solar irradiance satellite composite validation versus TSI proxy models. Astrophysics and Space Science 350(2), 421-442.

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Section: Resultscontrasting

confidence: 56%

ACRIM total solar irradiance satellite composite validation versus TSI proxy models

Scafetta

Willson²

2014

Astrophys Space Sci

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“…The implementation of SATIRE employing solar images in visible light and solar magnetograms (magnetic field intensity and polarity) is termed SATIRE-S (Wenzler et al, 2005;Ball et al, 2012;Yeo et al, 2014), and that based on the sunspot number (SSN) is SATIRE-T (Krivova et al, 2010). Individual records are accessible at http://www2.mps.mpg.…”

Section: Satirementioning

confidence: 99%

Solar forcing for CMIP6 (v3.2)

et al. 2017

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Abstract. This paper describes the recommended solar forcing dataset for CMIP6 and highlights changes with respect to CMIP5. The solar forcing is provided for radiative properties, namely total solar irradiance (TSI), solar spectral irradiance (SSI), and the F10.7 index as well as particle forcing, including geomagnetic indices Ap and Kp, and ionization rates to account for effects of solar protons, electrons, and galactic cosmic rays. This is the first time that a recommendation for solar-driven particle forcing has been provided for a CMIP exercise. The solar forcing datasets are provided at daily and monthly resolution separately for the CMIP6 preindustrial control, historical (1850CMIP6 preindustrial control, historical ( -2014, and future (2015-2300) simulations. For the preindustrial control simulation, both constant and time-varying solar forcing components are provided, with the latter including variability on 11-year and shorter timescales but no long-term changes. For the future, we provide a realistic scenario of what solar behavior could be, as well as an additional extreme Maunderminimum-like sensitivity scenario. This paper describes the forcing datasets and also provides detailed recommendations as to their implementation in current climate models.For the historical simulations, the TSI and SSI time series are defined as the average of two solar irradiance models that are adapted to CMIP6 needs: an empirical onePublished by Copernicus Publications on behalf of the European Geosciences Union. A new and lower TSI value is recommended: the contemporary solar-cycle average is now 1361.0 W m −2 . The slight negative trend in TSI over the three most recent solar cycles in the CMIP6 dataset leads to only a small global radiative forcing of −0.04 W m −2 . In the 200-400 nm wavelength range, which is important for ozone photochemistry, the CMIP6 solar forcing dataset shows a larger solar-cycle variability contribution to TSI than in CMIP5 (50 % compared to 35 %).We compare the climatic effects of the CMIP6 solar forcing dataset to its CMIP5 predecessor by using timeslice experiments of two chemistry-climate models and a reference radiative transfer model. The differences in the long-term mean SSI in the CMIP6 dataset, compared to CMIP5, impact on climatological stratospheric conditions (lower shortwave heating rates of −0.35 K day −1 at the stratopause), cooler stratospheric temperatures (−1.5 K in the upper stratosphere), lower ozone abundances in the lower stratosphere (−3 %), and higher ozone abundances (+1.5 % in the upper stratosphere and lower mesosphere). Between the maximum and minimum phases of the 11-year solar cycle, there is an increase in shortwave heating rates (+0.2 K day −1 at the stratopause), temperatures (∼ 1 K at the stratopause), and ozone (+2.5 % in the upper stratosphere) in the tropical upper stratosphere using the CMIP6 forcing dataset. This solar-cycle response is slightly larger, but not statistically significantly different from that for the CMIP5 forcing dataset.CMIP6 models wi...

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“…Here I k (λ, r) is the emergent intensity from the component k at the wavelength λ along the direction r. The functions α k (t, r) are the fractional coverages of the solar disc by the component k along the direction r, so that α k (t, r) dΩ gives the elementary solid angle covered by the component k. The two main building blocks of our model are the spectra I k (λ, r) and the fractional coverages α k (t, r) of the quiet Sun and magnetic features. We utilise the fractional coverages deduced by Ball et al (2012) from the full-disc continuum images and magnetograms obtained by the Michelson Doppler Imager onboard the Solar and Heliospheric Observatory (SOHO/MDI; Scherrer et al 1995). Ball et al (2012) successfully used these fractional coverages to reproduce 96% of TSI variations during cycle 23 (represented by the PMOD composite by Fröhlich 2006).…”

Section: The Modelmentioning

confidence: 99%

“…We utilise the fractional coverages deduced by Ball et al (2012) from the full-disc continuum images and magnetograms obtained by the Michelson Doppler Imager onboard the Solar and Heliospheric Observatory (SOHO/MDI; Scherrer et al 1995). Ball et al (2012) successfully used these fractional coverages to reproduce 96% of TSI variations during cycle 23 (represented by the PMOD composite by Fröhlich 2006). Following Ball et al (2011Ball et al ( , 2012 we replace the integration in Eq.…”

Section: The Modelmentioning

confidence: 99%

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The role of the Fraunhofer lines in solar brightness variability

Шапиро

Solanki

Krivova

et al. 2015

A&A

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Context. The solar brightness varies on timescales from minutes to decades. A clear identification of the physical processes behind such variations is needed for developing and improving physics-based models of solar brightness variability and reconstructing solar brightness in the past. This is, in turn, important for better understanding the solar-terrestrial and solar-stellar connections. Aims. We estimate the relative contributions of the continuum, molecular, and atomic lines to the solar brightness variations on different timescales. Methods. Our approach is based on the assumption that variability of the solar brightness on timescales greater than a day is driven by the evolution of the solar surface magnetic field. We calculated the solar brightness variations employing the solar disc area coverage of magnetic features deduced from the MDI/SOHO observations. The brightness contrasts of magnetic features relative to the quiet Sun were calculated with a non-LTE radiative transfer code as functions of disc position and wavelength. By consecutive elimination of molecular and atomic lines from the radiative transfer calculations, we assessed the role of these lines in producing solar brightness variability. Results. We show that the variations in Fraunhofer lines define the amplitude of the solar brightness variability on timescales greater than a day and even the phase of the total solar irradiance variability over the 11-year cycle. We also demonstrate that molecular lines make substantial contribution to solar brightness variability on the 11-year activity cycle and centennial timescales. In particular, our model indicates that roughly a quarter of the total solar irradiance variability over the 11-year cycle originates in molecular lines. The maximum of the absolute spectral brightness variability on timescales greater than a day is associated with the CN violet system between 380 and 390 nm.

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Reconstruction of total solar irradiance 1974–2009

Cited by 108 publications

References 46 publications

ACRIM total solar irradiance satellite composite validation versus TSI proxy models

ACRIM total solar irradiance satellite composite validation versus TSI proxy models

Solar forcing for CMIP6 (v3.2)

The role of the Fraunhofer lines in solar brightness variability

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