| Revision as of 18:33, 21 February 2005 editSEWilco (talk | contribs)Extended confirmed users, Pending changes reviewers24,018 edits →History of study of solar variations: Replaced stub section with summary of history of the field← Previous edit | Latest revision as of 16:19, 14 July 2021 edit undoTom.Reding (talk | contribs)Autopatrolled, Extended confirmed users, Page movers, Template editors3,879,760 editsm +{{Authority control}} (1 ID from Wikidata), WP:GenFixes on (uncategorized page)Tag: AWB | ||
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| '''Solar variation''' refers to fluctuation in the amount of energy emitted by the ]. Small variations have been measured from satellites during recent decades. Of interest to climate scientists is whether these variations have a significant effect on the temperature of the earth's atmosphere. | |||
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| The amount of ] emitted at the surface does not change much (see ]) from an average value of 1366 W/m². The variations in total output are so slight (as a percentage of total output) that they remained at or below the threshold of detectability until the satellite era, although the small fraction in ultra-violet wavelengths varies by a few percent. Total solar output is now measured to vary (over the last two 11-year sunspot cycles) by less that 0.1% or about 1 W/m² peak-to-trough of the 11 year sunspot cycle. There are no direct measurements of the longer-term variation and interpretations of ] measures of variations differ. Nonetheless, some theorise that solar variation is the primary cause of ]. | |||
| == Sunspots and Solar luminosity == | |||
| ]s are relatively dark areas on the surface of the Sun and are thus cooler than its average surface. The number of sunspots correlates with the intensity of solar radiation. Since sunspots are dark it is natural to assume that more sunspots means less solar radiation. However the surrounding areas are brighter and the overall effect is that more sunspots means a brighter sun. The variation is small (of the order of 1 W/m² or 0.1% of the total) and was only established once satellite measurements of solar variation became available in the 1980s. Various studies have been made using sunspot number (for which records extend over hundreds of years) as a ] for solar output (for which good records only extend for a few decades). Also, comparisons between ground instruments, high-altitude instruments, and instruments in orbit have been used to calibrate ground instruments. Researchers have combined present readings and factors to adjust historical data. Also used have been proxy data, such as measurements of cosmic ray isotopes to infer solar magnetic activity and thus the likely brightness. | |||
| ] | |||
| ==Solar cycles== | |||
| ]s are cyclic changes in behavior of the Sun. Many possible patterns have been noticed. | |||
| * 11 years: Most obvious is a gradual increase and decrease of the number of sunspots over a period of about 11 years, called the Schwabe cycle. This seems to be due to a shedding of entangled ]s. The Sun's surface is also the most active when there are more sunspots, although the ] does not change much due to an increase in bright spots (]). | |||
| * 22 years: Hale cycle. The magnetic field of the Sun reverses during each Schwabe cycle, so the magnetic poles return to the same state after two reversals. | |||
| * 88 years: Gleissberg cycle (70-100 years) is thought to be an amplitude modulation of the 11-year Schwabe Cycle (Sonnett and Finney, 1990). | |||
| * 200 years: Suess cycle. | |||
| * 2,000 years: Hallstadtzeit cycle. | |||
| * Other patterns have been detected: | |||
| ** In ]: 105, 131, 232, 385, 504, 805, 2,241 years (Damon and Sonnett, 1991). | |||
| ** During the ] 240 million years ago, mineral layers created in the Castile Formation show cycles of 2,500 years. | |||
| ==Solar irradiance of Earth and its surface== | |||
| ] is the amount of sunlight which reaches the Earth. The equipment used might measure optical brightness, total radiation, or radiation in various frequencies. Historical estimates use various measurements and proxies. | |||
| There are two common meanings: | |||
| * the radiation reaching the upper atmosphere | |||
| * the radiation reaching some point within the atmosphere, including the surface. | |||
| Various gases within the atmosphere absorb some solar radiation at different wavelengths, and clouds and dust also affect it. Hence measurements above the atmosphere are needed to observe variations in solar output, within the confounding effects of changes to the atmosphere. Indeed, there is some evidence that sunshine at the Earth's surface has been decreasing in the last 50 years (see ]) possibly caused by increased atmospheric pollution, whilst over roughly the same timespan solar output has been nearly constant. | |||
| ==Other effects due to solar variation== | |||
| Interaction of solar particles, the solar magnetic field, and the Earth's magnetic field, cause variations in the particle and electromagnetic fields at the surface of the planet. Extreme solar events can affect electrical devices. Weakening of the Sun's magnetic field is believed to increase the number of interstellar ] which reach Earth's atmosphere, altering the types of particles reaching the surface. It has been speculated that a change in cosmic rays could cause an increase in certain types of clouds, affecting Earth's ]. | |||
| == Global warming == | |||
| Some researchers have correlated solar variation with changes in the ]'s average temperature and ] - sometimes finding an effect, and sometimes not. When effects are found they have tended to be greater than can be explained by direct response to the change in radiative forcing from solar change, so some kind of feedback or amplification mechanism is required. See ] for a discussion of attribution of causes of current ]. | |||
| Research by ] and ] presents evidence that variations in solar radiation produced the warming that "put the green in ]" and led to a "]". The ]'s estimate of solar forcing since 1750 is available . | |||
| == Solar variation in climate models == | |||
| ] | |||
| ] are computer simulations which are used to examine understanding of climate behavior. Some models use constant values for solar irradiance, while some include the heating effects of a variable Sun. A good simulation by GCMs of global mean temperature over the last 100 years requires both natural (solar; volcanic) and human (]) factors. | |||
| There is currently no clear agreement as to the likely magnitude of long-term (last hundred or more years) solar variation. The ] discuss this in section 6.11 of the ] and show various results including Lean et al. (1995) . More recently Lean et al (GRL 2002, ) say: | |||
| : ''Our simulation suggests that secular changes in terrestrial proxies of solar activity (such as the 14C and 10Be cosmogenic isotopes and the aa geomagnetic index) can occur in the absence of long-term (i.e., secular) solar irradiance changes. ...this suggests that total solar irradiance may also lack significant secular trends. ...Solar radiative forcing of climate is reduced by a factor of 5 when the background component is omitted from historical reconstructions of total solar irradiance ...This suggest that general circulation model (GCM) simulations of twentieth century warming may overestimate the role of solar irradiance variability. ...There is, however, growing empirical evidence for the Sun's role in climate change on multiple time scales including the 11-year cycle ...Climate response to solar variability may involve amplification of climate modes which the GCMs do not typically include. ...In this way, long-term climate change may appear to track the amplitude of the solar activity cycles because the stochastic response increases with the cycle amplitude, not because there is an actual secular irradiance change.'' | |||
| == History of study of solar variations == | |||
| The longest recorded aspect of solar variations are changes in sunspots. Shortly after ]s began using the ] in ], sunspots and their motions were observed. Initial study was focused on their nature and behavior. Although the physical aspects of sunspots was not identified until the ]s, observations continued. Study was hampered during the ]s and ]s due to the low number of sunspots during what is now recognized as an extended period of low solar activity, this event named the ]. By the ]s records of their numbers began to show variations in their numbers. | |||
| For details about sunspots see the main article: ''']''' | |||
| Around ] connections between solar variations and weather on Earth began to be explored. Challenges are shown in the efforts of ], assigned by the ] to detect changes in the radiation of the Sun. His team had to begin by inventing instruments to measure solar radiation. Later, when he was head of the '''SAO''', it established a solar station at ], ] to complement its data from ]. He detected 27 harmonic periods within the 273-month Hale cycles, including 7, 13, and 39 month patterns. He looked for connections to weather by means such as matching opposing solar trends during a month to opposing temperature and precipitation trends in cities. | |||
| Statistical studies of solar activity with ] and ] were particularly popular until the ]s, when publications blossomed with studies of weather fronts and global ] patterns. Photos from space and ]s emphasized the importance of clouds and weather fronts. ] and ] have been enhanced by increasing use of ]s, beginning with simple ]s and replacing "]" values with more detailed solar variation as computing power increased and understanding of weather processes improves. | |||
| ==See Also== | |||
| * ] | |||
| ==External links== | |||
| * The Variable Sun - The American Institute of Physics. http://www.aip.org/history/climate/solar.htm | |||
| * Gerrit Lohmann, Norel Rimbu, Mihai Dima (2004). . International Journal of Climatology 24(8), 1045-1056 - Abstract: http://www.palmod.uni-bremen.de/~gerrit/abstractSolar.html | |||
| * Solar Climatic Effects (Recent Influence) – Summary. ]. ] ]. http://www.co2science.org/subject/s/summaries/solarrecin.htm | |||
| * S.K Solanski, M. Fligge (2001) ESA SP-463, ESA Publications Division. http://www.astro.phys.ethz.ch/papers/fligge/solspa_2.pdf | |||
| * S.K. Solanki, M. Fligge (2000) Space Science Review 94, 127-138 http://www.astro.phys.ethz.ch/papers/fligge/solfli_rev.pdf | |||
| * George C. Reid (1995) Aeronomy Laboratory, NOAA/ERL, Boulder, Colorado. U.S. National Report to IUGG, 1991-1994 Rev. Geophys. Vol. 33 Suppl. http://www.agu.org/revgeophys/reid00/reid00.html | |||
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