Convection zone
From Wikipedia, the free encyclopedia
The convection zone is the outermost layer of the Sun's interior. Energy is transferred there in convection currents, rather than energetic photons. Once hot gas convects up to the photosphere, it emits photons into space, cools, and settles back into the Sun. This convective flow is the origin of solar granules, and the departing energy is the visible light and other electromagnetic radiation that the Sun emits into space. (A good example of convection current is a lava lamp.)
| Image:Sun picture.png |
| Structure: Solar Core - Radiation Zone - Convection Zone |
| Atmosphere - Photosphere - Chromosphere - Transition region - Corona |
| Extended Structure: Termination Shock - Heliosphere - Heliopause - Heliosheath - Bow Shock |
| Solar Phenomena: Sunspots - Faculae - Granules - Supergranulation - Solar Wind - Spicules |
| Solar flares - Solar Prominences - Coronal Mass Ejections |
| Other: Solar System - Solar Variation - Solar Dynamo - Heliospheric Current Sheet - Solar Radiation - Solar Eclipse |
| The Sun is also occasionally referred to by its Latin name: Sol. |
