Final answer:
Energy is generated in the Sun's core through hydrogen fusion and moves outward via radiation and convection. The radiation zone handles energy transfer up to about 70% of the way to the Sun's surface, where it then switches to convection until it reaches the photosphere. The Sun's chromosphere and corona are the outer atmospheres, with phenomena like solar flares and prominences.
Step-by-step explanation:
To illustrate how energy moves from the Sun's core to its surface, let's start with the innermost part of the Sun. In the core, which contains about one-third of the Sun's mass, hydrogen fusion generates energy. This energy is then transferred outward primarily by two methods: radiation and convection.
Up until about 70% of the way from the center to the surface, energy is moved outward through radiation. This is where photons are absorbed and emitted in a random walk process. Once reaching the radiation zone's outer limit, energy transfer switches to the convection method. This is where convection currents carry the energy the rest of the way. Hotter material rises to the surface, cools down, and then sinks back to absorb more heat.
The Sun's surface, known as the photosphere, is where this energy finally becomes the sunlight we see. Above the photosphere are the chromosphere and the corona, which though not directly involved in energy transportation, are important for solar phenomena like solar flares and coronal mass ejections. Features such as coronal holes and prominences are also commonly observed in these regions.