Step 1: Understanding the Concept:
This problem describes quantum tunneling into a potential barrier. When a particle with energy \(E\) encounters a potential barrier \(V_0\) where \(E < V_0\), its wavefunction does not drop to zero immediately at the boundary but decays exponentially into the barrier. The probability density, which is the square of the wavefunction's magnitude, also decays exponentially.
Step 2: Key Formula or Approach:
In the classically forbidden region (\(x > 0\)), the wavefunction \(\psi(x)\) has the form: \[ \psi(x) = A e^{-\kappa x} \] The probability density is \(P(x) = |\psi(x)|^2 = |A|^2 e^{-2\kappa x}\). The decay constant \(\kappa\) is given by: \[ \kappa = \frac{\sqrt{2m(V_0 - E)}}{\hbar} \] where \(m\) is the mass of the particle. It is convenient to use relativistic units by rewriting \(\kappa\) as: \[ \kappa = \frac{\sqrt{2(mc^2)(V_0 - E)}}{\hbar c} \] Step 3: Detailed Explanation:
Given values: Particle energy, \(E = 8\) MeV. Potential height, \(V_0 = 48\) MeV. Neutron rest mass energy, \(mc^2 = 1\) GeV = 1000 MeV. \(\hbar c = 200\) MeV·fm. First, calculate the decay constant \(\kappa\): \[ V_0 - E = 48 \text{ MeV} - 8 \text{ MeV} = 40 \text{ MeV} \] \[ \kappa = \frac{\sqrt{2 \times (1000 \text{ MeV}) \times (40 \text{ MeV})}}{200 \text{ MeV fm}} = \frac{\sqrt{80000}}{200} \text{ fm}^{-1} \] \[ \kappa = \frac{\sqrt{16 \times 5000}}{200} = \frac{4 \sqrt{5000}}{200} = \frac{\sqrt{5000}}{50} = \frac{\sqrt{2500 \times 2}}{50} = \frac{50\sqrt{2}}{50} = \sqrt{2} \text{ fm}^{-1} \] So, \(\kappa \approx 1.414\) fm\(^{-1}\). The probability density \(P(x)\) decreases by a factor of 100 relative to its value at the boundary \(P(0)\): \[ \frac{P(x)}{P(0)} = \frac{|A|^2 e^{-2\kappa x}}{|A|^2 e^{0}} = e^{-2\kappa x} = \frac{1}{100} \] To find the distance \(x\), we solve for \(x\): \[ -2\kappa x = \ln\left(\frac{1}{100}\right) = -\ln(100) \] \[ x = \frac{\ln(100)}{2\kappa} \] Substitute the value of \(\kappa\): \[ x = \frac{\ln(100)}{2\sqrt{2}} \text{ fm} \] Using \(\ln(100) \approx 4.60517\) and \(\sqrt{2} \approx 1.41421\): \[ x \approx \frac{4.60517}{2 \times 1.41421} = \frac{4.60517}{2.82842} \approx 1.628 \text{ fm} \] Step 4: Final Answer:
The distance at which the probability density decreases by a factor of 100 is 1.63 fm.
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.)