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The sun emits maximum radiation of 0.52 micron meter. Assuming the sun to be a black body, Calculate the emissive ability of the sun’s surface at that temperature
- a)3.47 * 10 7 W/m2
- b)4.47 * 10 7 W/m2
- c)5.47 * 10 7 W/m2
- d)6.47 * 10 7 W/m2
Correct answer is option 'C'. Can you explain this answer?
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The sun emits maximum radiation of 0.52 micron meter. Assuming the sun...
E = σ b t 4 = 5.47 * 10 7 W/m2.
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The sun emits maximum radiation of 0.52 micron meter. Assuming the sun...
The emissive ability of a black body is given by the Stefan-Boltzmann law:
E = σT^4
where E is the emissive ability, σ is the Stefan-Boltzmann constant (5.67 x 10^-8 W/m^2K^4), and T is the temperature in Kelvin.
To calculate the emissive ability of the sun, we need to first convert the wavelength of maximum radiation (0.52 micrometer) to temperature using Wien's displacement law:
λmaxT = b
where b is a constant equal to 2.898 x 10^-3 mK. Solving for T:
T = b/λmax = (2.898 x 10^-3 mK)/(0.52 x 10^-6 m) = 5576 K
Now we can plug this temperature into the Stefan-Boltzmann law:
E = σT^4 = (5.67 x 10^-8 W/m^2K^4)(5576 K)^4 = 6.31 x 10^7 W/m^2
Therefore, the emissive ability of the sun is approximately 6.31 x 10^7 W/m^2.
E = σT^4
where E is the emissive ability, σ is the Stefan-Boltzmann constant (5.67 x 10^-8 W/m^2K^4), and T is the temperature in Kelvin.
To calculate the emissive ability of the sun, we need to first convert the wavelength of maximum radiation (0.52 micrometer) to temperature using Wien's displacement law:
λmaxT = b
where b is a constant equal to 2.898 x 10^-3 mK. Solving for T:
T = b/λmax = (2.898 x 10^-3 mK)/(0.52 x 10^-6 m) = 5576 K
Now we can plug this temperature into the Stefan-Boltzmann law:
E = σT^4 = (5.67 x 10^-8 W/m^2K^4)(5576 K)^4 = 6.31 x 10^7 W/m^2
Therefore, the emissive ability of the sun is approximately 6.31 x 10^7 W/m^2.
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