Faculae and Sunspots at Solar Maximum and Solar Minimum
The solar 'constant', the amount of energy received from the Sun during the course of the 11 year solar cycle, is not strictly constant. There is small variation during the course of the cycle due to the change in solar activity.
Sunspots form in regions with stronger magnetic fields on the photosphere and appear dark against the hotter solar surface, even though they are still quite hot. Faculae are extended regions that tend to form around sunspots and are hotter, and brighter, than the photosphere. Faculae are barely visible in solar imagery taken in visible light, but are more obvious in specific wavelengths (such as 1700 Angstroms used here) as the brighter speckled regions around many of the sunspots.
The hotter and more extended area of the faculae add more to the solar energy output than is taken away by the cooler and smaller sunspots, yielding a slight net increase in the solar luminosity around solar maximum.
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NASA's Scientific Visualization Studio
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Datasets used in this visualization
SDO SDO Continuum (Continuum)ID: 674Collected with HMI
SDO AIA 1700 (1700 Filter)ID: 710Collected with AIA JOINT SCIENCE OPERATIONS CENTER
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