The normalized ground-state wave function of a one-dimensional quantum harmonic oscillator with force constant \(K\) and mass \(m\) is \(\psi_0(x) = \left(\frac{\alpha}{\pi}\right)^{1/4} e^{-\alpha x^2/2}\), where \(\alpha = \frac{m\omega_0}{\hbar}\) and \(\omega_0^2 = \frac{K}{m}\). Which one of the following is the probability of finding the particle outside the classically allowed region?
(The classically allowed region is where the total energy is greater than the potential energy.)
Step 1: Determine classical turning point.
For ground state (\(n = 0\)), energy \(E_0 = \frac{1}{2}\hbar \omega_0\). Potential energy \(V(x) = \frac{1}{2}Kx^2 = \frac{1}{2}m\omega_0^2 x^2\). At the classical limit, \(V(x_c) = E_0 \Rightarrow x_c = \sqrt{\frac{\hbar}{m\omega_0}} = \frac{1}{\sqrt{\alpha}}\).
Step 2: Probability outside this region.
\[ P = 2 \int_{x_c}^{\infty} |\psi_0(x)|^2 dx = 2 \int_{x_c}^{\infty} \left(\frac{\alpha}{\pi}\right)^{1/2} e^{-\alpha x^2} dx \] Let \(y = \sqrt{\alpha} x \Rightarrow dy = \sqrt{\alpha} dx\): \[ P = \frac{2}{\sqrt{\pi}} \int_1^{\infty} e^{-y^2} dy \]
Step 3: Conclusion.
Hence, the probability outside the classically allowed region is \(\dfrac{2}{\sqrt{\pi}} \int_1^{\infty} e^{-y^2} dy\).

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.)