Step 1: Use boundary condition for magnetic fields.
The surface current density \(\vec{K}\) at the interface is given by:
\[
\mu_0 \vec{K} = \hat{n} \times (\vec{B_2} - \vec{B_1})
\]
Here, \(\hat{n}\) is the normal to the surface (along \(\hat{k}\)).
Step 2: Compute difference in magnetic fields.
\[
\vec{B_2} - \vec{B_1} = (8 - 3)\hat{i} + (3 - 5)\hat{j} + (5 - 0)\hat{k} = 5\hat{i} - 2\hat{j} + 5\hat{k}
\]
Step 3: Compute cross product.
\[
\hat{n} = \hat{k}
\]
\[
\hat{k} \times (\vec{B_2} - \vec{B_1}) = \hat{k} \times (5\hat{i} - 2\hat{j} + 5\hat{k}) = (2\hat{i} + 5\hat{j})
\]
\[
|\vec{K}| = \frac{1}{\mu_0} |\hat{n} \times (\vec{B_2} - \vec{B_1})| = \frac{1}{4\pi \times 10^{-7}} \sqrt{2^2 + 5^2} = \frac{5.385}{1.2566 \times 10^{-6}} = 4.28 \times 10^6
\]
\[ $\Rightarrow$ \alpha = 4.28
\]
Rounded to two decimals: \( \alpha = 4.28 \).
Step 4: Conclusion.
Hence, the surface current density magnitude is \(4.28 \times 10^6\, \text{A/m}\) and \(\alpha = 4.28.\)

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/m³, which is dimensionally incorrect for a spectral density. The correct unit J/(m³·Hz) or J·s/m³ is used here for the solution.)