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'''Granules''' on the [[photosphere]] of the [[Sun]] are caused by [[convection current]]s ([[thermal column]]s, [[Bénard cells]]) of [[Plasma (physics)|plasma]] within the Sun's convective zone. The grainy appearance of the solar photosphere is produced by the tops of these |
'''Granules''' on the [[photosphere]] of the [[Sun]] are caused by [[convection current]]s ([[thermal column]]s, [[Bénard cells]]) of [[Plasma (physics)|plasma]] within the Sun's convective zone. The grainy appearance of the solar photosphere is produced by the tops of these |
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The rising part of the center |
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potty where the [[plasma (physics)|plasma]] is hotter. The outer edge of the granules is darker due to the cooler descending plasma. (The terms ''darker'' and ''cooler'' are strictly by comparison to the brighter, hotter plasma. Since [[Stefan-Boltzmann equation|luminosity increases with the fourth power of temperature]], even a small loss of heat produces a large luminosity contrast; this "cooler", "darker" plasma is still far hotter and vastly brighter than a thermite reaction.) In addition to the visible appearance, which would be explained by [[convection|convective motion]], [[Doppler shift]] measurements of the light from individual granules provides evidence for the [[convective]] nature of the granules. |
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A typical granule has a diameter on the order of 1,500 kilometers<ref name="JBZ">{{cite book |
A typical granule has a diameter on the order of 1,500 kilometers<ref name="JBZ">{{cite book |
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Granules on the photosphere of the Sun are caused by convection currents (thermal columns, Bénard cells) of plasma within the Sun's convective zone. The grainy appearance of the solar photosphere is produced by the tops of these
The rising part of the center potty where the plasma is hotter. The outer edge of the granules is darker due to the cooler descending plasma. (The terms darker and cooler are strictly by comparison to the brighter, hotter plasma. Since luminosity increases with the fourth power of temperature, even a small loss of heat produces a large luminosity contrast; this "cooler", "darker" plasma is still far hotter and vastly brighter than a thermite reaction.) In addition to the visible appearance, which would be explained by convective motion, Doppler shift measurements of the light from individual granules provides evidence for the convective nature of the granules.
A typical granule has a diameter on the order of 1,500 kilometers[1] and lasts 8 to 20 minutes before dissipating.[2] At any one time, the Sun's surface is covered by about 4 million granules. Below the photosphere is a layer of "supergranules" up to 30,000 kilometers in diameter with lifespans of up to 24 hours.
