
The Lorentz transformation equations for space and time intervals are:
Ξt = Ξ³ (Ξtβ² + vΞxβ² / cΒ²)
Ξx = Ξ³ (Ξxβ² + vΞtβ²)
where:
Ξ³ = 1 / β(1 β vΒ² / cΒ²)
Ξ³ = 1 / β(1 β vΒ² / cΒ²)
= 1 / β(1 β (0.6)Β²)
= 1 / β(1 β 0.36) = 1 / β0.64 = 1.25
Using the Lorentz transformation for Ξt:
Ξt = Ξ³ Β· (vΞxβ² / cΒ²)
Substituting the values:
Ξt = 1.25 Γ (0.6c Γ 5) / cΒ²
= 1.25 Γ (3c / cΒ²)
= 1.25 Γ (3 Γ 10βΈ Γ 5) / (9 Γ 10ΒΉβΆ)
Simplify:
Ξt = (1.25 Γ 15) / (9 Γ 10βΈ)
= (1.25 Γ 5) / (3 Γ 10βΈ)
= 6.25 / (3 Γ 10βΈ)
Ξt = (6.25 / 3) ns = 12.5 ns
Using the Lorentz transformation for Ξx:
Ξx = Ξ³Ξxβ² = 1.25 Γ 5 = 6.25 m
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.)