A

To find the temperature of the sun, we can utilize the Stefan-Boltzmann Law, which states that the power radiated per unit area of a black body is proportional to the fourth power of its absolute temperature. The formula is given by:
P = \sigma imes T^4
Where:
- P is the power per unit area (W/m²)
- \sigma is the Stefan-Boltzmann constant (approximately 5.67 x 10^{-8} W/m² K⁴)
- T is the absolute temperature in Kelvin (K)
We are given that the solar constant is approximately 0.1 W/cm², which can be converted to W/m² as follows:
0.1 W/cm² = 0.1 imes 10^4 W/m² = 1000 W/m²
Now, substituting the values into the Stefan-Boltzmann Law:
1000 = 5.67 x 10^{-8} imes T^4
Rearranging for T:
T^4 = \frac{1000}{5.67 x 10^{-8}}
T^4 = 1.76 x 10^{10}
Taking the fourth root to find T:
T = (1.76 x 10^{10})^{1/4}
T \approx 238.2 K
Therefore, the temperature of the Sun, assuming it is a black body, is approximately 238.2 K.