149459
A body at $3000 \mathrm{~K}$ emits maximum energy at a wavelength of $9660 \AA$. If the sum emits maximum energy at a wavelength of $4950 \AA$. Then what would be the temperature of the sun?
A According to Wien's displacement law, the wavelength $\left(\lambda_{\mathrm{m}}\right)$ corresponding to which the energy emitted by a black body maximum is inversely proportional to its absolute temperature $(\mathrm{T})$. $\text { i.e., } \quad \lambda_{\mathrm{m}} \propto \frac{1}{\mathrm{~T}}$ $\lambda_{\mathrm{m}}=\frac{\mathrm{k}}{\mathrm{T}} \quad \text { [where, } \mathrm{k}=\text { Wien's constant] }$ $\lambda_{\mathrm{m}} \cdot \mathrm{T}=\mathrm{k}=\text { constant }$
AP EAMCET (21.09.2020) Shift-I
Heat Transfer
149465
The radiation emitted by a perfectly black body is proportional to
1 temperature on ideal gas scale
2 fourth root of temperature on ideal gas scale
3 fourth power of temperature on ideal gas scale
4 square of temperature on ideal gas scale
Explanation:
C Stefan's Boltzmann law states that total energy radiated per unit time is directly proportional to the fourth power of its absolute Temperature i.e. $E \propto T^{4}$ $E=\sigma T^{4}$ Where $\sigma$ is the Stefan's constant
BITSAT-2011
Heat Transfer
149467
The wavelength of radiation emitted by a body depends upon
1 the nature of its surface
2 the area of its surface
3 the temperature of its surface
4 All of the above
Explanation:
C According to Wein's displacement law $\lambda_{\mathrm{m}} \mathrm{T}=\text { Constant }$ $\lambda_{\mathrm{m}} \propto \frac{1}{\mathrm{~T}}$ Hence, the wavelength of radiation emitted by a body depends upon the temperature of the surface
149459
A body at $3000 \mathrm{~K}$ emits maximum energy at a wavelength of $9660 \AA$. If the sum emits maximum energy at a wavelength of $4950 \AA$. Then what would be the temperature of the sun?
A According to Wien's displacement law, the wavelength $\left(\lambda_{\mathrm{m}}\right)$ corresponding to which the energy emitted by a black body maximum is inversely proportional to its absolute temperature $(\mathrm{T})$. $\text { i.e., } \quad \lambda_{\mathrm{m}} \propto \frac{1}{\mathrm{~T}}$ $\lambda_{\mathrm{m}}=\frac{\mathrm{k}}{\mathrm{T}} \quad \text { [where, } \mathrm{k}=\text { Wien's constant] }$ $\lambda_{\mathrm{m}} \cdot \mathrm{T}=\mathrm{k}=\text { constant }$
AP EAMCET (21.09.2020) Shift-I
Heat Transfer
149465
The radiation emitted by a perfectly black body is proportional to
1 temperature on ideal gas scale
2 fourth root of temperature on ideal gas scale
3 fourth power of temperature on ideal gas scale
4 square of temperature on ideal gas scale
Explanation:
C Stefan's Boltzmann law states that total energy radiated per unit time is directly proportional to the fourth power of its absolute Temperature i.e. $E \propto T^{4}$ $E=\sigma T^{4}$ Where $\sigma$ is the Stefan's constant
BITSAT-2011
Heat Transfer
149467
The wavelength of radiation emitted by a body depends upon
1 the nature of its surface
2 the area of its surface
3 the temperature of its surface
4 All of the above
Explanation:
C According to Wein's displacement law $\lambda_{\mathrm{m}} \mathrm{T}=\text { Constant }$ $\lambda_{\mathrm{m}} \propto \frac{1}{\mathrm{~T}}$ Hence, the wavelength of radiation emitted by a body depends upon the temperature of the surface
149459
A body at $3000 \mathrm{~K}$ emits maximum energy at a wavelength of $9660 \AA$. If the sum emits maximum energy at a wavelength of $4950 \AA$. Then what would be the temperature of the sun?
A According to Wien's displacement law, the wavelength $\left(\lambda_{\mathrm{m}}\right)$ corresponding to which the energy emitted by a black body maximum is inversely proportional to its absolute temperature $(\mathrm{T})$. $\text { i.e., } \quad \lambda_{\mathrm{m}} \propto \frac{1}{\mathrm{~T}}$ $\lambda_{\mathrm{m}}=\frac{\mathrm{k}}{\mathrm{T}} \quad \text { [where, } \mathrm{k}=\text { Wien's constant] }$ $\lambda_{\mathrm{m}} \cdot \mathrm{T}=\mathrm{k}=\text { constant }$
AP EAMCET (21.09.2020) Shift-I
Heat Transfer
149465
The radiation emitted by a perfectly black body is proportional to
1 temperature on ideal gas scale
2 fourth root of temperature on ideal gas scale
3 fourth power of temperature on ideal gas scale
4 square of temperature on ideal gas scale
Explanation:
C Stefan's Boltzmann law states that total energy radiated per unit time is directly proportional to the fourth power of its absolute Temperature i.e. $E \propto T^{4}$ $E=\sigma T^{4}$ Where $\sigma$ is the Stefan's constant
BITSAT-2011
Heat Transfer
149467
The wavelength of radiation emitted by a body depends upon
1 the nature of its surface
2 the area of its surface
3 the temperature of its surface
4 All of the above
Explanation:
C According to Wein's displacement law $\lambda_{\mathrm{m}} \mathrm{T}=\text { Constant }$ $\lambda_{\mathrm{m}} \propto \frac{1}{\mathrm{~T}}$ Hence, the wavelength of radiation emitted by a body depends upon the temperature of the surface
149459
A body at $3000 \mathrm{~K}$ emits maximum energy at a wavelength of $9660 \AA$. If the sum emits maximum energy at a wavelength of $4950 \AA$. Then what would be the temperature of the sun?
A According to Wien's displacement law, the wavelength $\left(\lambda_{\mathrm{m}}\right)$ corresponding to which the energy emitted by a black body maximum is inversely proportional to its absolute temperature $(\mathrm{T})$. $\text { i.e., } \quad \lambda_{\mathrm{m}} \propto \frac{1}{\mathrm{~T}}$ $\lambda_{\mathrm{m}}=\frac{\mathrm{k}}{\mathrm{T}} \quad \text { [where, } \mathrm{k}=\text { Wien's constant] }$ $\lambda_{\mathrm{m}} \cdot \mathrm{T}=\mathrm{k}=\text { constant }$
AP EAMCET (21.09.2020) Shift-I
Heat Transfer
149465
The radiation emitted by a perfectly black body is proportional to
1 temperature on ideal gas scale
2 fourth root of temperature on ideal gas scale
3 fourth power of temperature on ideal gas scale
4 square of temperature on ideal gas scale
Explanation:
C Stefan's Boltzmann law states that total energy radiated per unit time is directly proportional to the fourth power of its absolute Temperature i.e. $E \propto T^{4}$ $E=\sigma T^{4}$ Where $\sigma$ is the Stefan's constant
BITSAT-2011
Heat Transfer
149467
The wavelength of radiation emitted by a body depends upon
1 the nature of its surface
2 the area of its surface
3 the temperature of its surface
4 All of the above
Explanation:
C According to Wein's displacement law $\lambda_{\mathrm{m}} \mathrm{T}=\text { Constant }$ $\lambda_{\mathrm{m}} \propto \frac{1}{\mathrm{~T}}$ Hence, the wavelength of radiation emitted by a body depends upon the temperature of the surface
