The phase difference \( \Delta \phi \) between the ordinary and extraordinary rays is given by: \[ \Delta \phi = \frac{2\pi}{\lambda_0} (n_e - n_o) \, d. \] For the light to remain linearly polarized, the phase difference must be a multiple of \( 2\pi \): \[ \Delta \phi = 2\pi m \quad \text{(where \( m \) is an integer)}. \]
Substituting \( \Delta \phi = 2\pi \) for the minimum thickness (i.e., \( m = 1 \)): \[ \frac{2\pi}{\lambda_0} (n_e - n_o) \, d = 2\pi. \] Simplify: \[ \frac{(n_e - n_o) \, d}{\lambda_0} = 1. \] Rearrange for \( d \): \[ d = \frac{\lambda_0}{n_e - n_o}. \]
Given: \[ \lambda_0 = 600 \, \text{nm} = 0.6 \, \mu\text{m}, \quad n_e - n_o = 0.05. \] Substitute into the formula: \[ d = \frac{0.6}{0.05} = 12 \, \mu\text{m}. \]
The plateβs thickness must account for half-wavelength retardation for the given wavelength, dividing \( d \) by 2: \[ d_{\text{min}} = \frac{12}{2} = 6 \, \mu\text{m}. \]
The minimum thickness of the plate is 6 Β΅m.
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.)