- 1(current)
Q. No.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. \(4 E\)
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1. \(1:4\)
2. \(3:1\)
3. \(1:2\)
4. \(6:1\)
| 1. | \((300)^1\) | 2. | \((300)^2\) |
| 3. | \((300)^3\) | 4. | \((300)^4\) |
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. | \((727)^4\) |
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1. \(100\)
2. \(200\)
3. \(400\)
4. \(800\)
| 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. | \(\left(\dfrac{4 \pi R^2 \times \sigma}{\alpha}\right)\) |
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- 1(current)
Q. No.
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