The radiative zone of the solar system comes immediately after the core, and its temperature is relatively lower, estimated at approximately three million degrees Celsius (Bruckner, 2013). Moreover, the density and pressure levels of the radiative zone are relatively lower than the conditions that occur within the solar core. Furthermore, the radiative layer comprises hydrogen and helium nuclei as well as free electrons (NASA, 2014). On the other hand, the third part of the solar structure is the convection layer, which occurs approximately 150,000 kilometers away from the sunâ€™s surface. Within this layer, temperatures are much lower, estimated at approximately one million degrees Kelvin (Bruckner, 2013). Moreover, within the convection layer, nuclei exist in close association with electrons and most atoms are undamaged or in gaseous form (NASA, 2014). The other important layer of the solar structure is the photosphere, which is the visible or the outermost part of the sun, and it extends several kilometers away from the other parts because of its gaseous nature
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