149494
The wavelength of maximum energy released during an atomic explosion was $2.93 \times 10^{-10} \mathrm{~m}$. The maximum temperature attained must be. (Wiens constant $=\mathbf{2 . 9 3} \times 10^{-3} \mathrm{mK}$ )
1 $5.86 \times 10^{7} \mathrm{~K}$
2 $10^{-13} \mathrm{~K}$
3 $10^{-7} \mathrm{~K}$
4 $10^{7} \mathrm{~K}$
Explanation:
D Given, $\lambda_{\mathrm{m}}=2.93 \times 10^{-10} \mathrm{~m}, \mathrm{~b}=2.93 \times 10^{-3}$ $\mathrm{mK}$ According to Wien's displacement law - $\lambda_{\mathrm{m}} \times \mathrm{T} =\mathrm{b}(\text { Constant })$ $\mathrm{T} =\frac{2.93 \times 10^{-3}}{2.93 \times 10^{-10}}=10^{7} \mathrm{~K}$
AIIMS-2010
Heat Transfer
149495
If the temperature of the sun were to increase from $T$ to $2 T$ and its radius from $R$ to $2 R$, then the ratio of the radiant energy received on earth to what it was previously will be
149499
A black body is at a temperature $300 \mathrm{~K}$. It emits energy at a rate, which is proportional to
1 $(300)^{4}$
2 $(300)^{3}$
3 $(300)^{2}$
4 300
Explanation:
A For black body radiation $\mathrm{E}=\sigma \mathrm{T}^{4}$ or $\mathrm{E} \propto \mathrm{T}^{4}$ Rate of emission of energy $\propto(300)^{4}$
AIIMS-2002
Heat Transfer
149528
The unit of Wien's constant $b$ is
1 $\mathrm{Wm}^{-2} \mathrm{~K}^{-4}$
2 $\mathrm{m}^{-1} \mathrm{~K}^{-1}$
3 $\mathrm{Wm}^{2}$
4 $\mathrm{m}-\mathrm{k}$
Explanation:
D According to Wein's displacement law $\lambda \mathrm{T}=$ constant Unit of Wein's constant $=$ unit of $\lambda \times$ unit of temperature $\mathrm{T}$ $=\mathrm{m}-\mathrm{K}$
MHT-CET 2009
Heat Transfer
149535
A hot body at temperature $T$ losses heat to the surrounding temperature $T_{s}$ by radiation. If the difference in the temperature is small then, the rate of loss of heat by the hot body is proportional to
A By the Newton's Law of cooling if the difference in the temperature is small then, the rate of loss of heat by the hot body is proportional to $\left(\mathrm{T}-\mathrm{T}_{\mathrm{s}}\right)$ According to Stefan's law, Energy radiated per second $\mathrm{E}=\frac{\mathrm{dT}}{\mathrm{dt}}=\sigma \varepsilon \mathrm{AT}^{4}$ When the temperature difference between the body and its surrounding is large $\frac{\mathrm{dT}}{\mathrm{dt}}=\sigma \varepsilon \Delta\left[\mathrm{T}^{4}-\mathrm{T}_{\mathrm{s}}^{4}\right]$
149494
The wavelength of maximum energy released during an atomic explosion was $2.93 \times 10^{-10} \mathrm{~m}$. The maximum temperature attained must be. (Wiens constant $=\mathbf{2 . 9 3} \times 10^{-3} \mathrm{mK}$ )
1 $5.86 \times 10^{7} \mathrm{~K}$
2 $10^{-13} \mathrm{~K}$
3 $10^{-7} \mathrm{~K}$
4 $10^{7} \mathrm{~K}$
Explanation:
D Given, $\lambda_{\mathrm{m}}=2.93 \times 10^{-10} \mathrm{~m}, \mathrm{~b}=2.93 \times 10^{-3}$ $\mathrm{mK}$ According to Wien's displacement law - $\lambda_{\mathrm{m}} \times \mathrm{T} =\mathrm{b}(\text { Constant })$ $\mathrm{T} =\frac{2.93 \times 10^{-3}}{2.93 \times 10^{-10}}=10^{7} \mathrm{~K}$
AIIMS-2010
Heat Transfer
149495
If the temperature of the sun were to increase from $T$ to $2 T$ and its radius from $R$ to $2 R$, then the ratio of the radiant energy received on earth to what it was previously will be
149499
A black body is at a temperature $300 \mathrm{~K}$. It emits energy at a rate, which is proportional to
1 $(300)^{4}$
2 $(300)^{3}$
3 $(300)^{2}$
4 300
Explanation:
A For black body radiation $\mathrm{E}=\sigma \mathrm{T}^{4}$ or $\mathrm{E} \propto \mathrm{T}^{4}$ Rate of emission of energy $\propto(300)^{4}$
AIIMS-2002
Heat Transfer
149528
The unit of Wien's constant $b$ is
1 $\mathrm{Wm}^{-2} \mathrm{~K}^{-4}$
2 $\mathrm{m}^{-1} \mathrm{~K}^{-1}$
3 $\mathrm{Wm}^{2}$
4 $\mathrm{m}-\mathrm{k}$
Explanation:
D According to Wein's displacement law $\lambda \mathrm{T}=$ constant Unit of Wein's constant $=$ unit of $\lambda \times$ unit of temperature $\mathrm{T}$ $=\mathrm{m}-\mathrm{K}$
MHT-CET 2009
Heat Transfer
149535
A hot body at temperature $T$ losses heat to the surrounding temperature $T_{s}$ by radiation. If the difference in the temperature is small then, the rate of loss of heat by the hot body is proportional to
A By the Newton's Law of cooling if the difference in the temperature is small then, the rate of loss of heat by the hot body is proportional to $\left(\mathrm{T}-\mathrm{T}_{\mathrm{s}}\right)$ According to Stefan's law, Energy radiated per second $\mathrm{E}=\frac{\mathrm{dT}}{\mathrm{dt}}=\sigma \varepsilon \mathrm{AT}^{4}$ When the temperature difference between the body and its surrounding is large $\frac{\mathrm{dT}}{\mathrm{dt}}=\sigma \varepsilon \Delta\left[\mathrm{T}^{4}-\mathrm{T}_{\mathrm{s}}^{4}\right]$
149494
The wavelength of maximum energy released during an atomic explosion was $2.93 \times 10^{-10} \mathrm{~m}$. The maximum temperature attained must be. (Wiens constant $=\mathbf{2 . 9 3} \times 10^{-3} \mathrm{mK}$ )
1 $5.86 \times 10^{7} \mathrm{~K}$
2 $10^{-13} \mathrm{~K}$
3 $10^{-7} \mathrm{~K}$
4 $10^{7} \mathrm{~K}$
Explanation:
D Given, $\lambda_{\mathrm{m}}=2.93 \times 10^{-10} \mathrm{~m}, \mathrm{~b}=2.93 \times 10^{-3}$ $\mathrm{mK}$ According to Wien's displacement law - $\lambda_{\mathrm{m}} \times \mathrm{T} =\mathrm{b}(\text { Constant })$ $\mathrm{T} =\frac{2.93 \times 10^{-3}}{2.93 \times 10^{-10}}=10^{7} \mathrm{~K}$
AIIMS-2010
Heat Transfer
149495
If the temperature of the sun were to increase from $T$ to $2 T$ and its radius from $R$ to $2 R$, then the ratio of the radiant energy received on earth to what it was previously will be
149499
A black body is at a temperature $300 \mathrm{~K}$. It emits energy at a rate, which is proportional to
1 $(300)^{4}$
2 $(300)^{3}$
3 $(300)^{2}$
4 300
Explanation:
A For black body radiation $\mathrm{E}=\sigma \mathrm{T}^{4}$ or $\mathrm{E} \propto \mathrm{T}^{4}$ Rate of emission of energy $\propto(300)^{4}$
AIIMS-2002
Heat Transfer
149528
The unit of Wien's constant $b$ is
1 $\mathrm{Wm}^{-2} \mathrm{~K}^{-4}$
2 $\mathrm{m}^{-1} \mathrm{~K}^{-1}$
3 $\mathrm{Wm}^{2}$
4 $\mathrm{m}-\mathrm{k}$
Explanation:
D According to Wein's displacement law $\lambda \mathrm{T}=$ constant Unit of Wein's constant $=$ unit of $\lambda \times$ unit of temperature $\mathrm{T}$ $=\mathrm{m}-\mathrm{K}$
MHT-CET 2009
Heat Transfer
149535
A hot body at temperature $T$ losses heat to the surrounding temperature $T_{s}$ by radiation. If the difference in the temperature is small then, the rate of loss of heat by the hot body is proportional to
A By the Newton's Law of cooling if the difference in the temperature is small then, the rate of loss of heat by the hot body is proportional to $\left(\mathrm{T}-\mathrm{T}_{\mathrm{s}}\right)$ According to Stefan's law, Energy radiated per second $\mathrm{E}=\frac{\mathrm{dT}}{\mathrm{dt}}=\sigma \varepsilon \mathrm{AT}^{4}$ When the temperature difference between the body and its surrounding is large $\frac{\mathrm{dT}}{\mathrm{dt}}=\sigma \varepsilon \Delta\left[\mathrm{T}^{4}-\mathrm{T}_{\mathrm{s}}^{4}\right]$
149494
The wavelength of maximum energy released during an atomic explosion was $2.93 \times 10^{-10} \mathrm{~m}$. The maximum temperature attained must be. (Wiens constant $=\mathbf{2 . 9 3} \times 10^{-3} \mathrm{mK}$ )
1 $5.86 \times 10^{7} \mathrm{~K}$
2 $10^{-13} \mathrm{~K}$
3 $10^{-7} \mathrm{~K}$
4 $10^{7} \mathrm{~K}$
Explanation:
D Given, $\lambda_{\mathrm{m}}=2.93 \times 10^{-10} \mathrm{~m}, \mathrm{~b}=2.93 \times 10^{-3}$ $\mathrm{mK}$ According to Wien's displacement law - $\lambda_{\mathrm{m}} \times \mathrm{T} =\mathrm{b}(\text { Constant })$ $\mathrm{T} =\frac{2.93 \times 10^{-3}}{2.93 \times 10^{-10}}=10^{7} \mathrm{~K}$
AIIMS-2010
Heat Transfer
149495
If the temperature of the sun were to increase from $T$ to $2 T$ and its radius from $R$ to $2 R$, then the ratio of the radiant energy received on earth to what it was previously will be
149499
A black body is at a temperature $300 \mathrm{~K}$. It emits energy at a rate, which is proportional to
1 $(300)^{4}$
2 $(300)^{3}$
3 $(300)^{2}$
4 300
Explanation:
A For black body radiation $\mathrm{E}=\sigma \mathrm{T}^{4}$ or $\mathrm{E} \propto \mathrm{T}^{4}$ Rate of emission of energy $\propto(300)^{4}$
AIIMS-2002
Heat Transfer
149528
The unit of Wien's constant $b$ is
1 $\mathrm{Wm}^{-2} \mathrm{~K}^{-4}$
2 $\mathrm{m}^{-1} \mathrm{~K}^{-1}$
3 $\mathrm{Wm}^{2}$
4 $\mathrm{m}-\mathrm{k}$
Explanation:
D According to Wein's displacement law $\lambda \mathrm{T}=$ constant Unit of Wein's constant $=$ unit of $\lambda \times$ unit of temperature $\mathrm{T}$ $=\mathrm{m}-\mathrm{K}$
MHT-CET 2009
Heat Transfer
149535
A hot body at temperature $T$ losses heat to the surrounding temperature $T_{s}$ by radiation. If the difference in the temperature is small then, the rate of loss of heat by the hot body is proportional to
A By the Newton's Law of cooling if the difference in the temperature is small then, the rate of loss of heat by the hot body is proportional to $\left(\mathrm{T}-\mathrm{T}_{\mathrm{s}}\right)$ According to Stefan's law, Energy radiated per second $\mathrm{E}=\frac{\mathrm{dT}}{\mathrm{dt}}=\sigma \varepsilon \mathrm{AT}^{4}$ When the temperature difference between the body and its surrounding is large $\frac{\mathrm{dT}}{\mathrm{dt}}=\sigma \varepsilon \Delta\left[\mathrm{T}^{4}-\mathrm{T}_{\mathrm{s}}^{4}\right]$
149494
The wavelength of maximum energy released during an atomic explosion was $2.93 \times 10^{-10} \mathrm{~m}$. The maximum temperature attained must be. (Wiens constant $=\mathbf{2 . 9 3} \times 10^{-3} \mathrm{mK}$ )
1 $5.86 \times 10^{7} \mathrm{~K}$
2 $10^{-13} \mathrm{~K}$
3 $10^{-7} \mathrm{~K}$
4 $10^{7} \mathrm{~K}$
Explanation:
D Given, $\lambda_{\mathrm{m}}=2.93 \times 10^{-10} \mathrm{~m}, \mathrm{~b}=2.93 \times 10^{-3}$ $\mathrm{mK}$ According to Wien's displacement law - $\lambda_{\mathrm{m}} \times \mathrm{T} =\mathrm{b}(\text { Constant })$ $\mathrm{T} =\frac{2.93 \times 10^{-3}}{2.93 \times 10^{-10}}=10^{7} \mathrm{~K}$
AIIMS-2010
Heat Transfer
149495
If the temperature of the sun were to increase from $T$ to $2 T$ and its radius from $R$ to $2 R$, then the ratio of the radiant energy received on earth to what it was previously will be
149499
A black body is at a temperature $300 \mathrm{~K}$. It emits energy at a rate, which is proportional to
1 $(300)^{4}$
2 $(300)^{3}$
3 $(300)^{2}$
4 300
Explanation:
A For black body radiation $\mathrm{E}=\sigma \mathrm{T}^{4}$ or $\mathrm{E} \propto \mathrm{T}^{4}$ Rate of emission of energy $\propto(300)^{4}$
AIIMS-2002
Heat Transfer
149528
The unit of Wien's constant $b$ is
1 $\mathrm{Wm}^{-2} \mathrm{~K}^{-4}$
2 $\mathrm{m}^{-1} \mathrm{~K}^{-1}$
3 $\mathrm{Wm}^{2}$
4 $\mathrm{m}-\mathrm{k}$
Explanation:
D According to Wein's displacement law $\lambda \mathrm{T}=$ constant Unit of Wein's constant $=$ unit of $\lambda \times$ unit of temperature $\mathrm{T}$ $=\mathrm{m}-\mathrm{K}$
MHT-CET 2009
Heat Transfer
149535
A hot body at temperature $T$ losses heat to the surrounding temperature $T_{s}$ by radiation. If the difference in the temperature is small then, the rate of loss of heat by the hot body is proportional to
A By the Newton's Law of cooling if the difference in the temperature is small then, the rate of loss of heat by the hot body is proportional to $\left(\mathrm{T}-\mathrm{T}_{\mathrm{s}}\right)$ According to Stefan's law, Energy radiated per second $\mathrm{E}=\frac{\mathrm{dT}}{\mathrm{dt}}=\sigma \varepsilon \mathrm{AT}^{4}$ When the temperature difference between the body and its surrounding is large $\frac{\mathrm{dT}}{\mathrm{dt}}=\sigma \varepsilon \Delta\left[\mathrm{T}^{4}-\mathrm{T}_{\mathrm{s}}^{4}\right]$
