Radiation energy corresponding to the temperature \(T\) of the sun is \(E.\) If its temperature is doubled, then its radiation energy will be:
1. \(32 E\)
2. \(16 E\)
3. \(8 E\)
4. \(4 E\)

Subtopic:  Stefan-Boltzmann Law |
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Level 1: 80%+
AIPMT - 1998
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Two spheres \(A\) and \(B\) of same material having radius \(8\) cm and \(4\) cm are maintained at temperatures \(127^{\circ}\text{C}\) and \(527^{\circ}\text{C}\) respectively. The ratio of energy radiated by \(A\) and \(B\) is:
1. \(1:4\)
2. \(3:1\)
3. \(1:2\)
4. \(6:1\)
Subtopic:  Stefan-Boltzmann Law |
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Level 1: 80%+
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A black body is at a temperature of \(300~ \text{K}.\) The rate at which it emits energy is proportional to:
1. \((300)^1\) 2. \((300)^2\)
3. \((300)^3\) 4. \((300)^4\)
Subtopic:  Stefan-Boltzmann Law |
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A black body is at \(727^\circ\text{C}.\) The rate at which it emits energy is proportional to:

1. \((727)^2\) 2. \((1000)^4\)
3. \((1000)^2\) 4. \((727)^4\)
Subtopic:  Stefan-Boltzmann Law |
 82%
Level 1: 80%+
AIPMT - 2007
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A spherical black body of radius \(10~\text{cm}\) radiates \(100~\text{W}\) power at \(400~\text K.\) If the radius were halved and the temperature doubled, the power radiated in watts would be:
1. \(100\)
2. \(200\)
3. \(400\)
4. \(800\)
Subtopic:  Stefan-Boltzmann Law |
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The radius of a spherical black body is \(R,\) and \(\alpha\) represents the rate of energy production within the body. The temperature of the given black body in a steady-state is: (where \(\sigma\) is Stefan- Boltzmann constant)
1. \(\left(\dfrac{\alpha}{\sigma \times 4 \pi R^2}\right)^{\dfrac{1}{4}} \) 2. \(\left(\dfrac{\sigma \times 4 \pi R^2}{\alpha}\right)^{\dfrac{1}{4}}\)
3. \(\left(\dfrac{\alpha}{\sigma \times 4 \pi R^2}\right)\) 4. \(\left(\dfrac{4 \pi R^2 \times \sigma}{\alpha}\right)\)
Subtopic:  Stefan-Boltzmann Law |
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Unit of Stefan's constant is:

1. Watt-m2-K4

2. Watt-m2/K4

3. Watt/m2–K

4. Watt/m2 K4

Subtopic:  Stefan-Boltzmann Law |
 80%
Level 1: 80%+
AIPMT - 2002
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