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The radiative zone is where energy produced in the core is transferred outward via radiation. Photons bounce around in this zone, taking a long time to reach the next layer, the convective zone.

The Sun's core is where nuclear fusion occurs, producing immense energy through the fusion of hydrogen atoms into helium. This process is critical for the Sun's energy output and supports all life on Earth.

In the convective zone, energy is transported by convection currents. Hot plasma rises, cools as it nears the surface, then falls back to be heated again, facilitating the transfer of energy to the photosphere.

The corona is the Sun's outer atmosphere, extremely hot and extending millions of kilometers into space. It can only be seen during a total solar eclipse and is the source of the solar wind.

The photosphere is the Sun's visible surface, where light is emitted that we can see. It's characterized by a granular appearance due to convective processes below it.

The chromosphere lies above the photosphere and is visible during solar eclipses as a red rim. It is a layer where solar prominences and flares may occur, affecting space weather.

CMEs are large expulsions of plasma and magnetic field from the Sun's corona. These space weather events can have significant effects on Earth's magnetosphere, potentially leading to geomagnetic storms.

The solar wind comprises streams of charged particles ejected from the corona. It interacts with planetary magnetic fields and can cause phenomena like auroras and geomagnetic storms on Earth.

Solar flares are sudden, intense bursts of radiation from the Sun's surface, caused by magnetic energy released in the chromosphere. They can disrupt communication systems and pose risks to satellites.