## Explanation

### Energy Transfer Overview

Energy generated in the core of the Sun is transferred to its outer layers through a series of complex processes. These can be broadly categorized into two primary mechanisms: **radiative transfer** and **convective transfer**. The transition between these two modes occurs at a region known as the **radiative-convective boundary**.

### Radiative Transfer

In the inner regions of the Sun, energy is moved outward primarily by **radiative diffusion**. Here, energy is carried by **photons**, which are particles of light. These photons are constantly absorbed and re-emitted by the surrounding particles. The process of radiative transfer can be described by the **radiative diffusion equation**:

Where:

- $I$ is the specific intensity
- $c$ is the speed of light
- $\mathbf{n}$ is the unit vector in the direction of photon travel
- $j$ is the emissivity
- $\alpha$ is the absorption coefficient

### Convective Transfer

As the energy moves outward and the temperature decreases, the efficiency of radiative transfer diminishes. Beyond the **radiative zone**, energy is primarily transferred by **convection**. This involves the physical movement of plasma. Hot plasma rises toward the outer layers, cools down, and then sinks back towards the inner layers. The efficiency of convection is usually described by the **convective heat transfer equation**:

Where:

- $q$ is the heat transferred per unit time
- $h_c$ is the convective heat transfer coefficient
- $A$ is the surface area through which convection occurs
- $\Delta T$ is the temperature difference

### Summary

In summary, energy produced in the Sun's core through nuclear fusion is transferred to its outer layers via **radiative diffusion** in the inner zones and **convective motions** in the outer zones. This intricate transfer of energy ensures that the Sun remains in a state of dynamic equilibrium, continuously supplying the energy that powers our solar system.