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The Sunspot Cycle

These two pictures of the Sun show how the number of sunspots changes. The picture on the left was taken near solar max in March 2001. It shows many sunspots. The picture on the right was taken near solar min in January 2005. It doesn't have any sunspots in it at all!
Click on image for full size (62K JPEG)
Images courtesy SOHO/NASA/ESA.
This graph shows the number of sunspots counted each year for many years. Can you see how the number of sunspots changes? Can you see the 11-year sunspot cycle?
Click on image for full size (8K GIF)
Windows to the Universe original artwork by Randy Russell.

The number of sunspots seen on the "surface" of the Sun changes from year to year. This rise and fall in sunspot counts is a cycle. The length of the cycle is about eleven years on average. The Sunspot Cycle was discovered in 1843 by the amateur German astronomer Samuel Heinrich Schwabe.

A peak in the sunspot count is called "solar maximum" (or "solar max"). The time when few sunspots appear is called a "solar minimum" (or "solar min"). An example of a recent sunspot cycle spans the years from the solar min in 1986, when 13 sunspots were seen, through the solar max in 1989 when more than 157 sunspots appeared, on to the next solar min in 1996 (ten years after the 1986 solar min) when the sunspot count had fallen back down to fewer than 9.

The length of the sunspot cycle is, on average, around eleven years. But the length of the cycle does vary. Between 1700 and today, the sunspot cycle (from one solar min to the next solar min) has varied in length from as short as nine years to as long as fourteen years.

Sometimes it is hard to get an exact count of number of sunspots on the Sun. Some spots are much bigger than others, some sunspots cross together at their edges, and many spots appear in groups. In 1848, a Swiss astronomer named Rudolf Wolf came up with the best way to count sunspots. The sunspot count using Wolf's formula, now known as the Wolf sunspot number, is still in use today. Wolf used data from earlier astronomers to reconstruct sunspot counts as far back as the 1755-1766 cycle, which he dubbed "cycle 1". Since then, subsequent cycles have been numbered consecutively, so the cycle that began with the 1996 solar minimum is cycle 23.

The Sun is usually very active when sunspot counts are high. Sunspots show us where the Sun's magnetic field might be "twisted up" enough to cause solar flares and coronal mass ejections. The Sun gives off more radiation than usual during solar max, and this extra energy changes the uppermost layers of Earth's atmosphere.


Sunspots

The Solar Cycle

History of Sunspot Observations

Activity: Graphing Sunspot Cycles

Movie: Magnetic Field Lines Tangle as Sun Rotates

Movie: Rotating Sun with Sunspots

Video: Dark Days Ahead for the Sun Movie: Dark Days Ahead for the Sun (RealVideo courtesy of the National Science Foundation)

Picture: Solar Corona at Solar Max and Solar Min

Picture: X-ray Image of the Sun at Solar Max and Solar Min

Sunspot Jigsaw Puzzle

Last modified October 27, 2006 by Randy Russell.

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Windows to the Universe, a project of the National Earth Science Teachers Association, is sponsored in part by the National Science Foundation and NASA, our Founding Partners (the American Geophysical Union and American Geosciences Institute) as well as through Institutional, Contributing, and Affiliate Partners, individual memberships and generous donors. Thank you for your support! NASA AGU AGI NSF