One of the most effective ways to understand the Sun's energy mechanism is to create a controllable simulation. The rate of nuclear fusion is not constant; it is highly dependent on the temperature and density (pressure) of the reaction environment. Higher temperatures cause atomic nuclei to move faster and collide more frequently; higher pressure brings the nuclei closer together, increasing the probability of collisions. These two factors together determine the number of fusion reactions per unit time, i.e., the power of energy produced. An ideal interactive model should allow visitors to simulate changes to these two core parameters through a simple control interface (such as rotating a handle), and observe in real-time changes in the fusion reaction rate (manifested as light intensity and particle animation speed) and energy output level, thus establishing a direct, quantifiable, and intuitive understanding of the relationship between "cause" and "effect." Operating our "Solar Fus
