(B) According to Wien's displacement law,the product of the wavelength of maximum intensity $(\lambda_m)$ and the absolute temperature $(T)$ is consta

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(B) According to Wien's displacement law,the product of the wavelength of maximum intensity $(\lambda_m)$ and the absolute temperature $(T)$ is constant.$\lambda_m T = \text{constant}$Therefore,$\lambda_{m1} T_1 = \lambda_{m2} T_2$Given: $\lambda_{m1} = 4800 \, \mathring{A}$,$T_1 = 6000 \, K$,$T_2 = 3000 \, K$.Substituting the values:$4800 \times 6000 = \lambda_{m2} \times 3000$$\lambda_{m2} = \frac{4800 \times 6000}{3000}$$\lambda_{m2} = 4800 \times 2 = 9600 \, \mathring{A}$.

Class 11 Physics 10-2.Heat Transfer Spectral Emissive Power and Wien's Displacement Law

Medium

Solar radiation emitted by the Sun resembles that of a black body at a temperature of $6000 \, K$. The maximum intensity of radiation is emitted at a wavelength of $4800 \, \mathring{A}$. If the temperature of the Sun decreases from $6000 \, K$ to $3000 \, K$,then at what wavelength (in $\mathring{A}$) will the maximum intensity of radiation be emitted?

A
$4800$
B
$9600$
C
$7200$
D
$6400$

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10-2.Heat Transfer

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Spectral Emissive Power and Wien's Displacement Law

The Earth radiates in the infra-red region of the spectrum. The spectrum is correctly given by

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The black discs $x, y$ and $z$ have radii $1 \ m, 2 \ m$ and $3 \ m$ respectively. The wavelengths corresponding to maximum intensity are $200 \ nm, 300 \ nm$ and $400 \ nm$ respectively. The relation between emissive power $E_{x}, E_{y}$ and $E_{z}$ is

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Star $S_1$ emits maximum radiation of wavelength $420 \, nm$ and the star $S_2$ emits maximum radiation of wavelength $560 \, nm$. What is the ratio of the temperature of $S_1$ and $S_2$?

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The wavelength of maximum intensity of radiation emitted by a star is $289.8 \, nm$. The radiation intensity for the star is: (Stefan's constant $\sigma = 5.67 \times 10^{-8} \, W m^{-2} K^{-4}$,Wien's constant $b = 2898 \, \mu m \cdot K$)

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If a black body is heated to a very high temperature,it appears to be:

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