1. Core:
* Density: 150 g/cm³ (about 150 times denser than water)
* Description: This is the heart of the Sun, where nuclear fusion takes place. It's the hottest and densest region, with intense pressure and temperature. It's where hydrogen is converted into helium, releasing immense energy that powers the Sun.
2. Radiative Zone:
* Density: 20 g/cm³ (gradually decreasing outward)
* Description: Energy from the core travels outward through this zone via radiation. Photons (light particles) are constantly absorbed and re-emitted by the dense plasma, taking a very long time to reach the next layer.
3. Convective Zone:
* Density: 0.2 g/cm³ (continues to decrease outward)
* Description: In this zone, energy is transported outward by convection. Hotter plasma rises, cools as it reaches the surface, and then sinks back down, creating a continuous cycle. This is the layer responsible for the Sun's "granulation," the mottled appearance of its surface.
4. Photosphere:
* Density: 0.0000002 g/cm³ (extremely thin compared to the interior)
* Description: This is the visible surface of the Sun, where sunlight is emitted into space. It's about 500 km thick.
5. Chromosphere:
* Density: 0.000000001 g/cm³ (even thinner than the photosphere)
* Description: A relatively thin layer above the photosphere, the chromosphere is characterized by spicules, jets of hot gas that extend upward. It's usually invisible, but can be seen during a total solar eclipse.
6. Transition Region:
* Density: Gradual transition between chromosphere and corona
* Description: This thin region marks a rapid temperature increase, transitioning from the chromosphere's cooler temperatures to the corona's extremely hot temperatures.
7. Corona:
* Density: Extremely low (only a few particles per cubic centimeter)
* Description: The outermost layer of the Sun's atmosphere, the corona is a vast and hot region extending millions of kilometers into space. It's responsible for the solar wind, a stream of charged particles that flows outward from the Sun.
Important Note: The densities given are approximate and can vary depending on location within each layer. Additionally, the Sun's structure is dynamic and can change over time due to various solar activities.
