The Taylor expansion of \( F(x) \) can be derived by multiplying the Taylor expansions of \( e^x \) and \( \sin x \).
\[ e^x = 1 + x + \frac{x^2}{2!} + \frac{x^3}{3!} + \frac{x^4}{4!} + \frac{x^5}{5!} + \dots \]
\[ \sin x = x - \frac{x^3}{3!} + \frac{x^5}{5!} - \dots \]
Multiply the two series and collect terms up to \( x^5 \):
\[ F(x) = \left( 1 + x + \frac{x^2}{2!} + \frac{x^3}{3!} + \frac{x^4}{4!} + \frac{x^5}{5!} \right) \cdot \left( x - \frac{x^3}{3!} + \frac{x^5}{5!} \right) \]
\[ \frac{1}{120} + \frac{1}{24} + \frac{1}{12} - \frac{1}{12} - \frac{1}{24} - \frac{1}{120} \]
\[ \frac{1}{120} - \frac{1}{120} + \frac{1}{24} - \frac{1}{24} + \frac{1}{12} - \frac{1}{12} = -\frac{1}{29.41} \approx -0.034 \]
The coefficient of \( x^5 \) in the Taylor expansion of \( F(x) = e^x \sin x \) is approximately \(-0.034\).
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.)