Modelling total solar irradiance since 1878 from simulated magnetograms

Dasi-Espuig, M.; Jiang, Jingyang; Krivova, N. A.; Solanki, S. K.

doi:10.1051/0004-6361/201424290

Cited by 34 publications

(60 citation statements)

References 88 publications

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“…The facular areas and positions were then computed based on the sunspot group areas and positions as described below. The model parameters used here are taken from observations and are the same as in Jiang et al (2011b) and Dasi-Espuig et al (2014).…”

Section: Active Region Fluxmentioning

confidence: 99%

“…Therefore, we linked the amplitude and length of the ephemeral region cycles to those of the corresponding sunspot cycles based on the R g record. The relationships that provide the link contain two free parameters: the amplitude, X, and the time extension, c x , of the ephemeral region cycles (for more details see Dasi-Espuig et al 2014).…”

Section: Ephemeral Region Fluxmentioning

confidence: 99%

“…We have updated the present study (with respect to Dasi-Espuig et al 2014) to obtain the magnetic flux from ephemeral regions corresponding to cycle 24, that are present during the end of cycle 23.…”

Section: Ephemeral Region Fluxmentioning

confidence: 99%

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Reconstruction of spectral solar irradiance since 1700 from simulated magnetograms

Dasi-Espuig

Jiang

Krivova

et al. 2016

A&A

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Aims. We present a reconstruction of the spectral solar irradiance since 1700 using the SATIRE-T2 (Spectral And Total Irradiance REconstructions for the Telescope era version 2) model. This model uses as input magnetograms simulated with a surface flux transport model fed with semi-synthetic records of emerging sunspot groups. Methods. The record of sunspot group areas and positions from the Royal Greenwich Observatory (RGO) is only available since 1874. We used statistical relationships between the properties of sunspot group emergence, such as the latitude, area, and tilt angle, and the sunspot cycle strength and phase to produce semi-synthetic sunspot group records starting in the year 1700. The semi-synthetic records are fed into a surface flux transport model to obtain daily simulated magnetograms that map the distribution of the magnetic flux in active regions (sunspots and faculae) and their decay products on the solar surface. The magnetic flux emerging in ephemeral regions is accounted for separately based on the concept of extended cycles whose length and amplitude are linked to those of the sunspot cycles through the sunspot number. The magnetic flux in each surface component (sunspots, faculae and network, and ephemeral regions) was used to compute the spectral and total solar irradiance (TSI) between the years 1700 and 2009. This reconstruction is aimed at timescales of months or longer although the model returns daily values. Results. We found that SATIRE-T2, besides reproducing other relevant observations such as the total magnetic flux, reconstructs the TSI on timescales of months or longer in good agreement with the PMOD composite of observations, as well as with the reconstruction starting in 1878 based on the RGO-SOON data. The model predicts an increase in the TSI of 1.2 +0.2 −0.3 Wm −2 between 1700 and the present. The spectral irradiance reconstruction is in good agreement with the UARS/SUSIM measurements as well as the Lyman-α composite.

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Section: Active Region Fluxmentioning

confidence: 99%

Section: Ephemeral Region Fluxmentioning

confidence: 99%

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Reconstruction of spectral solar irradiance since 1700 from simulated magnetograms

Dasi-Espuig

Jiang

Krivova

et al. 2016

A&A

Self Cite

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“…However, full-disc images of the Sun, typically used by such models, are only available for the last few decades. Reconstructions of past irradiance changes usually rely on observations of sunspots (Lean et al 1995;Solanki & Fligge 2000;Wang et al 2005;Krivova et al 2007Krivova et al , 2010Dasi-Espuig et al 2014, 2016, or concentrations of cosmogenic radionuclides, e.g. 14 C and 10 Be (Steinhilber et al 2009;Delaygue & Bard 2011;Shapiro et al 2011;Vieira et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Analysis of full disc Ca II K spectroheliograms

Chatzistergos

Ermolli

Solanki

et al. 2018

A&A

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Context. Historical Ca II K spectroheliograms (SHG) are unique in representing long-term variations of the solar chromospheric magnetic field. They usually suffer from numerous problems and lack photometric calibration. Thus accurate processing of these data is required to get meaningful results from their analysis. Aims. In this paper we aim at developing an automatic processing and photometric calibration method that provides precise and consistent results when applied to historical SHG. Methods. The proposed method is based on the assumption that the centre-to-limb variation of the intensity in quiet Sun regions does not vary with time. We tested the accuracy of the proposed method on various sets of synthetic images that mimic problems encountered in historical observations. We also tested our approach on a large sample of images randomly extracted from seven different SHG archives. Results. The tests carried out on the synthetic data show that the maximum relative errors of the method are generally <6.5%, while the average error is <1%, even if rather poor quality observations are considered. In the absence of strong artefacts the method returns images that differ from the ideal ones by <2% in any pixel. The method gives consistent values for both plage and network areas. We also show that our method returns consistent results for images from different SHG archives. Conclusions. Our tests show that the proposed method is more accurate than other methods presented in the literature. Our method can also be applied to process images from photographic archives of solar observations at other wavelengths than Ca II K.

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“…Energy from the Sun reaching the Earth drives almost every known physical and biological cycle in the Earth system. With the launch of the Hickey-Frieden cavity radiometer (HF) on Nimbus 7 in 1978 October, space-based observations have lasted more than 30 yr. Now it is well known that TSI varies on timescales of minutes to decades (even longer than several solar cycles; Willson & Hudson 1991;Fröhlich 2006Fröhlich , 2009Fröhlich , 2013Wenzler et al 2006;Kopp & Lean 2011;Li et al 2012;Dasi-Espuig et al 2014;Velasco Herrera et al 2015). TSI generates the Earth's radiation environment and influences its temperature and atmosphere;even asmall persistent variation of the solar irradiance takes part in climate changes, so it is very important for us to understand how the variations of TSI affect the Earth's climate system.…”

Section: Introductionmentioning

confidence: 99%

What Causes the Inter-Solar-Cycle Variation of Total Solar Irradiance?

Xiang

Kong

2015

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The Physikalisch Meteorologisches Observatorium Davos total solar irradiance (TSI), Active Cavity Radiometer Irradiance Monitoring TSI, and Royal Meteorological Institute of Belgium TSI are three typical TSI composites. Magnetic Plage Strength Index (MPSI) and Mount Wilson Sunspot Index (MWSI) should indicate the weak and strong magnetic field activity on the solar full disk, respectively. Cross-correlation (CC) analysis of MWSI with three TSI composites shows that TSI should be weakly correlated with MWSI, and not be in phase with MWSI at timescales of solar cycles. The wavelet coherence (WTC) and partial wavelet coherence (PWC) of TSI with MWSI indicate that the inter-solar-cycle variation of TSI is also not related to solar strong magnetic field activity, which is represented by MWSI. However, CC analysis of MPSI with three TSI composites indicates that TSI should be moderately correlated and accurately in phase with MPSI at timescales of solar cycles, and that the statisticalsignificancetest indicates that the correlation coefficient of three TSI composites with MPSI is statistically significantly higher than that of three TSI composites with MWSI. Furthermore, the cross wavelet transform (XWT) and WTC of TSI with MPSI show that the TSI is highly related and actually in phase with MPSI at a timescale of a solar cycle as well. Consequently, the CC analysis, XWT, and WTC indicate that the solar weak magnetic activity on the full disk, which is represented by MPSI, dominates the inter-solar-cycle variation of TSI.

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Modelling total solar irradiance since 1878 from simulated magnetograms

Cited by 34 publications

References 88 publications

Reconstruction of spectral solar irradiance since 1700 from simulated magnetograms

Reconstruction of spectral solar irradiance since 1700 from simulated magnetograms

Analysis of full disc Ca II K spectroheliograms

What Causes the Inter-Solar-Cycle Variation of Total Solar Irradiance?

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