If the radiant flux from the sun is 1350 W/m2, what would be its equivalent blackbody
temperature?
To calculate the equivalent blackbody temperature, we can use Stefan-Boltzmann Law.
The Stefan-Boltzmann Law states that the total radiant flux emitted by a perfect blackbody is proportional to the fourth power of its temperature (in Kelvin). Mathematically, it can be expressed as:
F = σ * T^4
Where:
F is the radiant flux (in Watts per square meter),
σ is the Stefan-Boltzmann constant (approximately 5.67 x 10^-8 Watts per square meter per Kelvin to the power of 4),
T is the temperature (in Kelvin) that we are trying to find.
In this case, the radiant flux (F) from the sun is given as 1350 W/m^2.
So, we can rearrange the equation to solve for T:
T^4 = F / σ
T^4 = 1350 / (5.67 x 10^-8)
T^4 ≈ 2.38492 x 10^16
Taking the fourth root of both sides, we can determine the value of T:
T ≈ ∛∛(2.38492 x 10^16)
T ≈ 424.5 Kelvin
Therefore, the equivalent blackbody temperature for a radiant flux of 1350 W/m^2 from the sun is approximately 424.5 Kelvin.