dc.contributor.author | Yndestad, Harald | |
dc.contributor.author | Solheim, Jan Erik | |
dc.date.accessioned | 2018-03-23T07:37:49Z | |
dc.date.available | 2018-03-23T07:37:49Z | |
dc.date.issued | 2017-08-30 | |
dc.description.abstract | Total solar irradiance (TSI) is the primary quantity of energy that is provided to the Earth. The properties
of the TSI variability are critical for understanding the cause of the irradiation variability and its expected
influence on climate variations. A deterministic property of TSI variability can provide information about
future irradiation variability and expected long-term climate variation, whereas a non-deterministic variability
can only explain the past.
This study of solar variability is based on an analysis of two TSI data series, one since 1700 A.D. and one
since 1000 A.D.; a sunspot data series since 1610 A.D.; and a solar orbit data series from 1000 A.D. The
study is based on a wavelet spectrum analysis. First, the TSI data series are transformed into a wavelet
spectrum. Then, the wavelet spectrum is transformed into an autocorrelation spectrum to identify stationary,
subharmonic and coincidence periods in the TSI variability.
The results indicate that the TSI and sunspot data series have periodic cycles that are correlated with
the oscillations of the solar position relative to the barycenter of the solar system, which is controlled by
gravity force variations from the large planets Jupiter, Saturn, Uranus and Neptune. A possible explanation
for solar activity variations is forced oscillations between the large planets and the solar dynamo.
We find that a stationary component of the solar variability is controlled by the 12-year Jupiter period
and the 84-year Uranus period with subharmonics. For TSI and sunspot variations, we find stationary periods
related to the 84-year Uranus period. Deterministic models based on the stationary periods confirm
the results through a close relation to known long solar minima since 1000 A.D. and suggest a modern
maximum period from 1940 to 2015. The model computes a new Dalton-type sunspot minimum from
approximately 2025 to 2050 and a new Dalton-type period TSI minimum from approximately 2040 to
2065. | en_US |
dc.description | Accepted manuscript version. Published version available in <a href=https://doi.org/10.1016/j.newast.2016.08.020> New Astronomy, 51, 135–152. </a> | en_US |
dc.identifier.citation | Yndestad, H. & Solheim, J. E. (2017) The influence of solar system oscillation on the variability of the total solar irradiance. New Astronomy, 51, 135-152. | en_US |
dc.identifier.cristinID | FRIDAID 1378510 | |
dc.identifier.doi | 10.1016/j.newast.2016.08.020 | |
dc.identifier.issn | 1384-1092 | |
dc.identifier.uri | https://hdl.handle.net/10037/12421 | |
dc.language.iso | eng | en_US |
dc.publisher | Elsevier | en_US |
dc.relation.journal | New Astronomy | |
dc.rights.accessRights | openAccess | en_US |
dc.subject | VDP::Matematikk og naturvitenskap: 400 | en_US |
dc.subject | VDP::Mathematics and natural scienses: 400 | en_US |
dc.subject | Grand minima / Grand minima | en_US |
dc.subject | Solar oscillation / Solar oscillation | en_US |
dc.subject | Wavelet analysis / Wavelet analysis | en_US |
dc.title | The influence of solar system oscillation on the variability of the total solar irradiance | en_US |
dc.type | Journal article | en_US |
dc.type | Tidsskriftartikkel | en_US |
dc.type | Peer reviewed | en_US |