Failụ si na nke mbu(1,813 × 762 pixel, ívù akwukwo orunótu: 115 KB, MIME nke: image/png)
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Mmẹkụwátá
This figure summarizes sunspot number observations. Since c. 1749, continuous monthly averages[dead link] of sunspot activity have been available and are shown here as reported by the Solar Influences Data Analysis Center, World Data Center for the Sunspot Index, at the Royal Observatory of Belgium. These figures are based on an average of measurements from many different observatories around the world. Prior to 1749, sporadic observations of sunspots are available. These were compiled and placed on consistent monthly framework by Hoyt & Schatten (1998a, 1998b).
The most prominent feature of this graph is the c. 11 year solar magnetic cycle which is associated with the natural waxing and waning of solar activity.
On longer time scales, the sun has shown considerable variability, including the long Maunder Minimum when almost no sunspots were observed, the less severe Dalton Minimum, and increased sunspot activity during the last fifty years, known as the Modern Maximum. The causes for these variations are not well understood, but because sunspots and associated faculae affect the brightness of the sun, solar luminosity is lower during periods of low sunspot activity. It is widely believed that the low solar activity during the Maunder Minimum may be among the principal causes of the chilly Little Ice Age, circa 1350-1850 A.D.
Copyright
This figure was prepared by Robert A. Rohde and is part of the Global Warming Art project.
Í nwèrèíkí jé, gbạsáa na/ma í mezí akwukwo nka na okpúrù íwú GNU Ákwúkwó Íwú nke Owéré, Nké 1.2 ma nke íchè ndi Free Software Foundation; wéfùtàrà; na adighi nkejị di íchẹ, adighi édé nke Ihú-Ihü Ákwúkwó, na adighi Ázú-Ihü Ákwúkwó. Ákwúkwó iwu hé jéré jé di na nkeji kpóró GNU Ákwúkwó Íwú nke Owéré".http://www.gnu.org/copyleft/fdl.htmlGFDLGNU Free Documentation Licensetruetrue
í-kpó-áhà – Ị ga-enyerịrị ugo kwesịrị ekwesị, nye njikọ na ikikere ahụ, ma gosikwa ma emere mgbanwe. Ị nwere ike ime ya n'ụzọ ezi uche ọ bụla, mana ọ bụghị n'ụzọ ọ bụla na-egosi na onye nyere ikikere kwadoro gị maọbụ ojiji gị.
gbásàa kà – Ọ bụrụ na ị tụgharịgharịa, gbanwee, ma ọ bụ wulite n'elu ihe ahụ, ị ga-ekesa ndenye gị n'okpuru otu ma ọ bụ ikike dakọtara dị ka nke mbụ.
This licensing tag was added to this file as part of the GFDL licensing update.http://creativecommons.org/licenses/by-sa/3.0/CC BY-SA 3.0Creative Commons Attribution-Share Alike 3.0truetrue
References
Hoyt, D. V., and K. H. Schatten (1998a). "Group sunspot numbers: A new solar activity reconstruction. Part 1.". Solar Physics179: 189-219.
Hoyt, D. V., and K. H. Schatten (1998b). "Group sunspot numbers: A new solar activity reconstruction. Part 2.". Solar Physics181: 491-512.
I added another decade to the graph (through Oct., 2015). I started with the previous version was uploaded in 2006. Because it was almost a decade old, it lacked Solar Cycle 24. So I started with that version, and pasted a properly-scaled version of h...
I added another decade to the graph (through Oct., 2015). I started with the previous version was uploaded in 2006. Because it was almost a decade old, it lacked Solar Cycle 24. So I started with that version, and pasted a properly-scaled version of h...