Volume 544, August 2012
|Number of page(s)||6|
|Published online||02 August 2012|
Confronting a solar irradiance reconstruction with solar and stellar data
1 High Altitude Observatory, National Center for Atmospheric Research, PO Box 3000, Boulder, CO 80307-3000, USA ⋆
The National Center for Atmospheric Research is sponsored by the National Science Foundation.
2 Lowell Observatory, 1400 Mars Hill Road, Flagstaff, AZ 86001, USA
3 Air Force Research Laboratory, National Solar Observatory, Sunspot NM 88349, USA
4 Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Blvd., Box 9501, Nashville, TN 37209, USA
5 Physikalisch-Meteorologishes Observatorium Davos, World Radiation Center, 7260 Davos Dorf, Switzerland
6 NorthWest Research Associates, 3380 Mitchell Lane, Boulder, CO 80301, USA
Received: 27 January 2012
Accepted: 6 June 2012
Context. A recent paper by Shapiro and colleagues (2011, A&A, 529, A67) reconstructs spectral and total irradiance variations of the Sun during the holocene.
Aims. In this note, we comment on why their methodology leads to large (0.5%) variations in the solar TSI on century-long time scales, in stark contrast to other reconstructions which have ≲ 0.1% variations.
Methods. We examine the amplitude of the irradiance variations from the point of view of both solar and stellar data.
Results. Shapiro et al.’s large amplitudes arise from differences between the irradiances computed from models A and C of Fontenla and colleagues, and from their explicit assumption that the radiances of the quiet Sun vary with the cosmic ray modulation potential. We suggest that the upper photosphere, as given by model A, is too cool, and discuss relative contributions of local vs. global dynamos to the magnetism and irradiance of the quiet Sun. We compare the slow (>22 yr) components of the irradiance reconstructions with secular changes in stellar photometric data that span 20 years or less, and find that the Sun, if varying with such large amplitudes, would still lie within the distribution of stellar photometric variations measured over a 10−20 year period. However, the stellar time series are individually too short to see if the reconstructed variations will remain consistent with stellar variations when observed for several decades more.
Conclusions. By adopting model A, Shapiro et al. have over-estimated quiet-Sun irradiance variations by about a factor of two, based upon a re-analysis of sub-mm data from the James Clerk Maxwell telescope. But both estimates are within bounds set by current stellar data. It is therefore vital to continue accurate photometry of solar-like stars for at least another decade, to reveal secular and cyclic variations on multi-decadal time scales of direct interest to the Sun.
Key words: Sun: activity / Sun: surface magnetism / solar-terrestrial relations
© ESO, 2012
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