\(\text{Zero}\)
\(-\frac{1}{r^4}\)
The vector field is \( \mathbf{F} = \frac{\mathbf{r}}{r^3} \), where \( \mathbf{r} = r\hat{r} \) and \( r = \sqrt{x^2 + y^2 + z^2} \). Using the divergence formula:
\[ \nabla \cdot \mathbf{F} = \frac{\partial F_x}{\partial x} + \frac{\partial F_y}{\partial y} + \frac{\partial F_z}{\partial z}, \] after computing partial derivatives and simplifying, we find:
\[ \nabla \cdot \mathbf{F} = 0. \]
Final Answer: The divergence of \( \frac{\hat{r}}{r^3} \) is Zero.
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.)