Question

The wavelength at which the Sun emits its most intense light is about $550 \mathrm{nm}$. Assuming the Sun radiates as a perfect black body, estimate (a) its surface tempera ture and (b) its total emitted power. [Hint: The Sun's data can be found in the inside back cover of the book.

Name: Problem 10, Chapter 27: College Physics
Uploaded: 2021-05-05T10:39:12-08:00
Duration: 2 min 11 s
Channel: Sheh Lit Chang
Description: The wavelength at which the Sun emits its most intense light is about 550 nm. Assuming the Sun radiates as a perfect black body, estimate (a) its surface tempera ture and (b) its total emitted power. [Hint: The Sun's data can be found in the inside back cover of the book.

   The wavelength at which the Sun emits its most intense light is about $550 \mathrm{nm}$. Assuming the Sun radiates as a perfect black body, estimate (a) its surface tempera ture and (b) its total emitted power. [Hint: The Sun's data can be found in the inside back cover of the book.

College Physics

Jerry D. Wilson,… 7th Edition

Chapter 27, Problem 10

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Solved by Expert Sheh Lit Chang

05/05/2021

Step 1

We can use Wien's displacement law to estimate the surface temperature of the Sun. Wien's displacement law is given by: \[ \lambda_{\text{max}} T = 2.90 \times 10^{-3} \, \text{m} \cdot \text{K} \] where $\lambda_{\text{max}}$ is the wavelength at which the Show more…

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The wavelength at which the Sun emits its most intense light is about $550 \mathrm{nm}$. Assuming the Sun radiates as a perfect black body, estimate (a) its surface tempera ture and (b) its total emitted power. [Hint: The Sun's data can be found in the inside back cover of the book.

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Key Concepts

Blackbody Radiation

This principle describes an idealized object that absorbs all incident electromagnetic radiation and re-emits energy in a characteristic continuous spectrum that depends solely on its temperature. It serves as a fundamental model for understanding the thermal emission of stars and other astronomical bodies.

Wien's Displacement Law

This law relates the temperature of a blackbody to the wavelength at which its emission is most intense. It shows that as the temperature increases, the peak wavelength shifts to shorter values, thereby allowing the determination of the temperature from the peak emission wavelength.

Stefan-Boltzmann Law

This law states that the total energy radiated per unit surface area of a blackbody is proportional to the fourth power of its absolute temperature. It is essential for estimating the total power output or luminosity of an object from its temperature.

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