J/A+A/531/A6 Evolution of solar irradiance during Holocene (Vieira+, 2011)
Evolution of the solar irradiance during the Holocene.
Vieira L.E.A., Solanki S.K., Krivova N.A., Usoskin I.
<Astron. Astrophys. 531, A6 (2011)>
=2011A&A...531A...6V 2011A&A...531A...6V
ADC_Keywords: Sun ; Earth
Keywords: Sun: activity - Sun: faculae, plages - Sun: surface magnetism -
solar-terrestrial relations - sunspots - Sun: UV radiation
Abstract:
Long-term records of solar radiative output are vital for
understanding solar variability and past climate change. Measurements
of solar irradiance are available for only the last three decades,
which calls for reconstructions of this quantity over longer time
scales using suitable models.
We present a physically consistent reconstruction of the total solar
irradiance for the Holocene.
Description:
This is a composite total solar irradiance (TSI) time series for
9495BC to 2007AD constructed as described in Sect. 3.3 of the paper.
Since the TSI is the main external heat input into the Earth's climate
system, a consistent record covering as long period as possible is
needed for climate models. This was our main motivation for
constructing this composite TSI time series.
In order to produce a representative time series, we divided the
Holocene into four periods according to the available data for each
period. Table 4 (see below) summarizes the periods considered and the
models available for each period. After the end of the Maunder Minimum
we compute daily values, while prior to the end of the Maunder Minimum
we compute 10-year averages. For the period for which both solar disk
magnetograms and continuum images are available (period 1) we employ
the SATIRE-S reconstruction (Krivova et al. 2003A&A...399L...1K 2003A&A...399L...1K;
Wenzler et al. 2006A&A...460..583W 2006A&A...460..583W). SATIRE-T (Krivova et al.
2010JGRA..11512112K 2010JGRA..11512112K) reconstruction is used from the beginning of
the Maunder Minimum (approximately 1640AD) to 1977AD. Prior to 1640AD
reconstructions are based on cosmogenic isotopes (this paper).
Different models of the Earth's geomagnetic field are available before
and after approximately 5000BC. Therefore we treat periods 3 and 4
(before and after 5000BC) separately. Further details can be found in
the paper. We emphasize that the reconstructions based on different
proxies have different time resolutions.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tsi_hol.dat 46 136619 Total Solar Irradiance (TSI) evolution during
the Holocene
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Table 4: SATIRE Models employed to construct a representative TSI time series
for the Holocene.
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Index Period Cadence Model Input Data
-------------------------------------------------------------------------
1 1974AD - 2010AD Daily SATIRE-S Full disk magnetograms and continuum
images
2 1640AD - 1974AD Daily SATIRE-T Sunspot observations
3 5000BC - 1640AD Decadal SATIRE-M Cosmogenic isotopes (14C; VADM
and VDM geomagnetic field)
4 9495BC - 5000BC Decadal SATIRE-M Cosmogenic isotopes (14C; VADM
geomagnetic field)
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Note: We replaced missing values from 1
From 1974AD to 1977 missing values computed employing SATIRE-S were replaced
by SaTIRE-T.
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Byte-by-byte Description of file: tsi_hol.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Date Date (YYYYY/MM/DD)
13- 23 F11.5 W/m2 TSI ?=-9999.9 Total solar irradiance (1)
25- 35 F11.5 W/m2 TSI10 ?=-9999.9 Total solar irradiance
(10-year running after 1640AD) (1)
37- 44 F8.5 W/m2 e_TSI ?=-9.9 1-sigma error on TSI
46 I1 --- Model [1/9] Model (2)
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Note (1): SATIRE (Spectral and Total Irradiance Reconstructions) TSI composite.
Note (2): Models as follows:
1 = SATIRE-S, which models the irradiance during the satellite era
with high precision (in its present version since 1974)
2 = SATIRE-T, which computes irradiance during the telescope era
(since 1610)
3 = SATIRE-M, M for millennial time scales
9 = NA
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Acknowledgements:
Luis Eduardo Vieira, luis.vieira(at)cnrs-orleans.fr
(End) Luis Eduardo Vieira [LPC2E], Patricia Vannier [CDS] 26-May-2011