02. Radiation
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Heat Transfer

149449 Power emitted by a black body at temperature $50^{\circ} \mathrm{C}$ is $\mathrm{P}$. Now, temperature is doubled i.e. temperature of black body becomes $100^{\circ} \mathrm{C}$. Now, power emitted is

1 greater than $\mathrm{P}$ but less than $16 \mathrm{P}$
2 greater than 16P
3 $\mathrm{P}$
4 $16 \mathrm{P}$
UPSEE - 2017
Heat Transfer

149451 The intensity of radiation emitted by two stars $A$ and $B$ are in the ratio of $16: 1$. The wavelength corresponding to their peak emission of radiation will be in the ratio of

1 $2: 1$
2 $4: 1$
3 $1: 2$
4 $16: 1$
UPSEE - 2011
Heat Transfer

149452 The intensity of radiation emitted by the sun has its maximum value at a wavelength of 510 nm and that emitted by the north star has the maximum value at wavelength of $350 \mathrm{~nm}$. If these stars behave like black bodies, then the ratio of surface temperatures of the sun and north star is

1 1.46
2 0.69
3 1.21
4 0.83
UPSEE - 2008
Heat Transfer

149453 Assuming the sun to have a spherical outer surface of radius $r$, radiating like a black body at temperature $t^{\circ} \mathrm{C}$, the power received by a unit surface, (normal to the incident rays) at a distance $R$ from the centre of the sun is

1 $\frac{4 \pi r^{2} \sigma t^{4}}{R^{2}}$
2 $\frac{r^{2} \sigma(t+273)^{4}}{4 \pi R^{2}}$
3 $\frac{16 \pi^{2} r^{2} \sigma t^{4}}{R^{2}}$
4 $\frac{r^{2} \sigma(t+273)^{4}}{R^{2}}$
UPSEE - 2007
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Heat Transfer

149449 Power emitted by a black body at temperature $50^{\circ} \mathrm{C}$ is $\mathrm{P}$. Now, temperature is doubled i.e. temperature of black body becomes $100^{\circ} \mathrm{C}$. Now, power emitted is

1 greater than $\mathrm{P}$ but less than $16 \mathrm{P}$
2 greater than 16P
3 $\mathrm{P}$
4 $16 \mathrm{P}$
UPSEE - 2017
Heat Transfer

149451 The intensity of radiation emitted by two stars $A$ and $B$ are in the ratio of $16: 1$. The wavelength corresponding to their peak emission of radiation will be in the ratio of

1 $2: 1$
2 $4: 1$
3 $1: 2$
4 $16: 1$
UPSEE - 2011
Heat Transfer

149452 The intensity of radiation emitted by the sun has its maximum value at a wavelength of 510 nm and that emitted by the north star has the maximum value at wavelength of $350 \mathrm{~nm}$. If these stars behave like black bodies, then the ratio of surface temperatures of the sun and north star is

1 1.46
2 0.69
3 1.21
4 0.83
UPSEE - 2008
Heat Transfer

149453 Assuming the sun to have a spherical outer surface of radius $r$, radiating like a black body at temperature $t^{\circ} \mathrm{C}$, the power received by a unit surface, (normal to the incident rays) at a distance $R$ from the centre of the sun is

1 $\frac{4 \pi r^{2} \sigma t^{4}}{R^{2}}$
2 $\frac{r^{2} \sigma(t+273)^{4}}{4 \pi R^{2}}$
3 $\frac{16 \pi^{2} r^{2} \sigma t^{4}}{R^{2}}$
4 $\frac{r^{2} \sigma(t+273)^{4}}{R^{2}}$
UPSEE - 2007
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Heat Transfer

149449 Power emitted by a black body at temperature $50^{\circ} \mathrm{C}$ is $\mathrm{P}$. Now, temperature is doubled i.e. temperature of black body becomes $100^{\circ} \mathrm{C}$. Now, power emitted is

1 greater than $\mathrm{P}$ but less than $16 \mathrm{P}$
2 greater than 16P
3 $\mathrm{P}$
4 $16 \mathrm{P}$
UPSEE - 2017
Heat Transfer

149451 The intensity of radiation emitted by two stars $A$ and $B$ are in the ratio of $16: 1$. The wavelength corresponding to their peak emission of radiation will be in the ratio of

1 $2: 1$
2 $4: 1$
3 $1: 2$
4 $16: 1$
UPSEE - 2011
Heat Transfer

149452 The intensity of radiation emitted by the sun has its maximum value at a wavelength of 510 nm and that emitted by the north star has the maximum value at wavelength of $350 \mathrm{~nm}$. If these stars behave like black bodies, then the ratio of surface temperatures of the sun and north star is

1 1.46
2 0.69
3 1.21
4 0.83
UPSEE - 2008
Heat Transfer

149453 Assuming the sun to have a spherical outer surface of radius $r$, radiating like a black body at temperature $t^{\circ} \mathrm{C}$, the power received by a unit surface, (normal to the incident rays) at a distance $R$ from the centre of the sun is

1 $\frac{4 \pi r^{2} \sigma t^{4}}{R^{2}}$
2 $\frac{r^{2} \sigma(t+273)^{4}}{4 \pi R^{2}}$
3 $\frac{16 \pi^{2} r^{2} \sigma t^{4}}{R^{2}}$
4 $\frac{r^{2} \sigma(t+273)^{4}}{R^{2}}$
UPSEE - 2007
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Heat Transfer

149449 Power emitted by a black body at temperature $50^{\circ} \mathrm{C}$ is $\mathrm{P}$. Now, temperature is doubled i.e. temperature of black body becomes $100^{\circ} \mathrm{C}$. Now, power emitted is

1 greater than $\mathrm{P}$ but less than $16 \mathrm{P}$
2 greater than 16P
3 $\mathrm{P}$
4 $16 \mathrm{P}$
UPSEE - 2017
Heat Transfer

149451 The intensity of radiation emitted by two stars $A$ and $B$ are in the ratio of $16: 1$. The wavelength corresponding to their peak emission of radiation will be in the ratio of

1 $2: 1$
2 $4: 1$
3 $1: 2$
4 $16: 1$
UPSEE - 2011
Heat Transfer

149452 The intensity of radiation emitted by the sun has its maximum value at a wavelength of 510 nm and that emitted by the north star has the maximum value at wavelength of $350 \mathrm{~nm}$. If these stars behave like black bodies, then the ratio of surface temperatures of the sun and north star is

1 1.46
2 0.69
3 1.21
4 0.83
UPSEE - 2008
Heat Transfer

149453 Assuming the sun to have a spherical outer surface of radius $r$, radiating like a black body at temperature $t^{\circ} \mathrm{C}$, the power received by a unit surface, (normal to the incident rays) at a distance $R$ from the centre of the sun is

1 $\frac{4 \pi r^{2} \sigma t^{4}}{R^{2}}$
2 $\frac{r^{2} \sigma(t+273)^{4}}{4 \pi R^{2}}$
3 $\frac{16 \pi^{2} r^{2} \sigma t^{4}}{R^{2}}$
4 $\frac{r^{2} \sigma(t+273)^{4}}{R^{2}}$
UPSEE - 2007
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