* Core: This is the very center of the Sun, where nuclear fusion occurs. It is incredibly dense and hot, reaching temperatures of around 15 million degrees Celsius. This is where hydrogen atoms fuse into helium, releasing immense energy that powers the Sun.
* Radiative Zone: This region surrounds the core and extends outward for about 70% of the Sun's radius. Energy from the core travels outwards through this zone as electromagnetic radiation, specifically photons. This process can take hundreds of thousands of years due to the dense plasma of the zone.
* Convective Zone: This region lies above the radiative zone and extends to the Sun's surface. Here, energy is transported by convection, where hot gas rises to the surface, cools, and sinks back down. This creates a churning motion that can be seen as granulation on the Sun's surface.
* Photosphere: This is the visible surface of the Sun, where the light we see originates. It is about 500 kilometers thick and has a temperature of around 5,500 degrees Celsius.
* Chromosphere: This layer lies above the photosphere and is only visible during a total solar eclipse. It is a thin layer of hot gas that extends several thousand kilometers into space. The chromosphere is home to spicules, jets of hot gas that shoot up from the photosphere.
* Corona: This outermost region of the Sun's atmosphere extends millions of kilometers into space. It is incredibly hot, reaching temperatures of millions of degrees Celsius. The corona is responsible for the solar wind, a stream of charged particles that flows outward from the Sun.
These are the main regions of the Sun, each with its own unique characteristics and role in the Sun's activity.
