1. Core:
* Location: Deepest layer at the Sun's center.
* Temperature: Around 15 million degrees Celsius (27 million degrees Fahrenheit).
* Density: Extremely dense, over 150 times denser than water.
* Processes: Nuclear fusion occurs here, converting hydrogen into helium and releasing immense energy in the form of light and heat. This is the source of the Sun's energy.
2. Radiative Zone:
* Location: Extends from the core to about 70% of the Sun's radius.
* Temperature: Gradually decreases from the core to about 2 million degrees Celsius (3.6 million degrees Fahrenheit).
* Density: Decreases with distance from the core.
* Processes: Energy from the core is transported outwards primarily by radiation, meaning photons are absorbed and re-emitted by the dense plasma. This process is extremely slow, taking millions of years for energy to reach the surface.
3. Convective Zone:
* Location: Extends from the radiative zone to the Sun's surface, about 200,000 km deep.
* Temperature: Decreases further to around 5,500 degrees Celsius (9,932 degrees Fahrenheit).
* Density: Less dense than the radiative zone.
* Processes: Energy is transported outwards by convection, meaning hotter, less dense plasma rises and cooler, denser plasma sinks. This process is much faster than radiation and creates the boiling appearance seen at the surface.
4. Photosphere:
* Location: The visible surface of the Sun.
* Temperature: Around 5,500 degrees Celsius (9,932 degrees Fahrenheit).
* Density: Much thinner than the interior layers, but still much denser than air.
* Processes: This is where light and heat energy finally escape the Sun. The photosphere appears granular due to the convection cells below. Sunspots, cooler regions, and solar flares occur in this layer.
5. Chromosphere:
* Location: A thin layer above the photosphere.
* Temperature: Increases with height, reaching around 100,000 degrees Celsius (180,000 degrees Fahrenheit).
* Density: Very thin.
* Processes: The chromosphere is characterized by spicules, small, jet-like eruptions of hot plasma. Solar flares and prominences can extend into this layer.
6. Corona:
* Location: The outermost layer of the Sun's atmosphere, extending millions of kilometers into space.
* Temperature: Extremely high, reaching millions of degrees Celsius (millions of degrees Fahrenheit).
* Density: Extremely thin.
* Processes: The corona is heated by magnetic energy, and the exact mechanisms are still being studied. It is responsible for the solar wind, a stream of charged particles that flows outward from the Sun.
These are the major layers of the Sun, each playing a critical role in its structure and energy production. While it might seem like a simple ball of gas, the Sun is a complex and dynamic system with a lot of fascinating features.
