Let the distance of the axis from the center of mass of the hemisphere be \( d \). Using the parallel axis theorem, the moment of inertia about the given axis can be expressed as:
\[ I = I_{\text{CM}} + M d^2 \]
where:
\[ I_{\text{CM}} = \text{moment of inertia of the hemisphere about the axis through its center of mass}. \]
For a solid hemisphere, the moment of inertia about an axis through its center of mass and parallel to the flat surface is:
\[ I_{\text{CM}} = \frac{83}{320} M R^2 \]
Substituting \( I = \frac{2}{5} M R^2 \) into the equation:
\[ \frac{2}{5} M R^2 = \frac{83}{320} M R^2 + M d^2 \]
Dividing throughout by \( M R^2 \):
\[ \frac{2}{5} = \frac{83}{320} + d^2 \]
Rearranging:
\[ d^2 = \frac{2}{5} - \frac{83}{320} \]
Converting fractions to a common denominator:
\[ \frac{2}{5} = \frac{128}{320} \]
\[ d^2 = \frac{128}{320} - \frac{83}{320} = \frac{45}{320} \]
Taking the square root:
\[ d = \sqrt{\frac{45}{320}} \]
Breaking it down:
\[ d = \frac{\sqrt{45}}{\sqrt{320}} = \frac{3\sqrt{5}}{8\sqrt{2}} = \frac{3\sqrt{10}}{16} \]
Approximating the value:
\[ d \approx 0.375 R \]
Thus, the distance of the axis from the center of mass is \( d \approx 0.375 R \).
In order to achieve the static equilibrium of the see-saw about the fulcrum \( P \), shown in the figure, the weight of Box B should be _________ kg, if the weight of Box A is 50 kg.
A particle of mass 1kg, initially at rest, starts sliding down from the top of a frictionless inclined plane of angle \(\frac{π}{6}\)\(\frac{\pi}{6}\) (as schematically shown in the figure). The magnitude of the torque on the particle about the point O after a time 2seconds is ______N-m. (Rounded off to nearest integer)
(Take g = 10m/s2)
At a particular temperature T, Planck's energy density of black body radiation in terms of frequency is \(\rho_T(\nu) = 8 \times 10^{-18} \text{ J/m}^3 \text{ Hz}^{-1}\) at \(\nu = 3 \times 10^{14}\) Hz. Then Planck's energy density \(\rho_T(\lambda)\) at the corresponding wavelength (\(\lambda\)) has the value \rule{1cm}{0.15mm} \(\times 10^2 \text{ J/m}^4\). (in integer)
[Speed of light \(c = 3 \times 10^8\) m/s]
(Note: The unit for \(\rho_T(\nu)\) in the original problem was given as J/mΒ³, which is dimensionally incorrect for a spectral density. The correct unit J/(mΒ³Β·Hz) or JΒ·s/mΒ³ is used here for the solution.)