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Consider two single-particle states, \(A\) and \(B,\) in a system of fermions, where \(\epsilon_{A}=\mu-x\) and \(\epsilon_{B}=\mu+x ;\) that is, level \(A\) lies below \(\mu\) by the same amount that level \(B\) lies above \(\mu\). Prove that the probability of level \(B\) being occupied is the same as the probability of level \(A\) being unoccupied. In other words, the Fermi-Dirac distribution is "symmetrical" about the point where \(\epsilon=\mu\).

Short Answer

Expert verified
The Fermi-Dirac distribution shows symmetry about \( \epsilon = \mu \) as \( f(\epsilon_B) = 1 - f(\epsilon_A) \).

Step by step solution

01

Identify the Fermi-Dirac Distribution

The probability that a fermion state of energy \( \epsilon \) is occupied is given by the Fermi-Dirac distribution: \[ f(\epsilon) = \frac{1}{e^{(\epsilon - \mu)/kT} + 1} \] where \( \mu \) is the chemical potential and \( kT \) is the thermal energy.
02

Calculate the Probability of Level A Being Occupied

For level \( A \), the energy is \( \epsilon_A = \mu - x \). So, we have the probability of occupation as: \[ f(\epsilon_A) = \frac{1}{e^{(-x)/kT} + 1} = \frac{1}{e^{-x/kT} + 1} \] This represents the probability that level \( A \) is occupied.
03

Calculate the Probability of Level A Being Unoccupied

The probability of a level being unoccupied is \( 1 \) minus the probability of it being occupied. For level \( A \), this is: \[ 1 - f(\epsilon_A) = 1 - \frac{1}{e^{-x/kT} + 1} = \frac{e^{-x/kT}}{e^{-x/kT} + 1} \]
04

Calculate the Probability of Level B Being Occupied

For level \( B \), the energy is \( \epsilon_B = \mu + x \). So, the probability of occupation is: \[ f(\epsilon_B) = \frac{1}{e^{x/kT} + 1} \] This represents the probability that level \( B \) is occupied.
05

Show Probability Symmetry

Notice that: \[ f(\epsilon_B) = \frac{1}{e^{x/kT} + 1} = \frac{e^{-x/kT}}{e^{-x/kT} + 1} \] which is exactly the probability \( 1 - f(\epsilon_A) \) found in Step 3. This symmetry shows that the probability of level \( B \) being occupied is equal to the probability of level \( A \) being unoccupied.

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Key Concepts

These are the key concepts you need to understand to accurately answer the question.

Fermionic States
In the world of quantum physics, fermionic states refer to the states that follow Fermi-Dirac statistics. These states are occupied by particles known as fermions. Fermions are particles that obey the Pauli exclusion principle, which means that no two fermions can occupy the same quantum state simultaneously. Electrons, protons, and neutrons are examples of fermions. This property is critical in understanding the behavior of particles in atoms and solids.

Fermionic states can exist in various energy levels. When considering these levels around the chemical potential, it becomes crucial to apply the Fermi-Dirac distribution. The distribution functions describe the probability of each energy level being occupied by a fermion. This concept helps explain phenomena such as electrical conductivity and the characteristics of metals and insulators at different temperatures.
Chemical Potential
The chemical potential, denoted by \( \mu \), is a fundamental concept in thermodynamics and quantum mechanics. It represents the change in the system's energy when adding a particle, keeping the volume and entropy constant. In practical terms, the chemical potential can be thought of as the energy level at which the system is equally likely to gain or lose a particle.

In the Fermi-Dirac distribution, the chemical potential plays a vital role in determining the distribution of particles among energy states. During experiments or calculations, the chemical potential helps identify at which energy levels fermions predominantly reside and how these distributions adjust with temperature changes. In metals, \( \mu \) is closely related to the Fermi energy, a critical factor influencing their electronic properties.
  • It sets the reference point around which energies are considered.
  • It determines the probability of occupation when compared to specific state energies.
Thermal Energy
Thermal energy is the energy that comes from the temperature of matter. It's a concept that links the thermal motion of particles with their physical and chemical properties. In terms like \( kT \), where \( k \) is the Boltzmann constant and \( T \) is the temperature, thermal energy becomes part of the discussion in quantum mechanics and statistical physics.

When considering the Fermi-Dirac distribution, thermal energy affects how "sharp" the transition is between occupied and unoccupied states near the chemical potential. At absolute zero temperature, fermionic states below the chemical potential are fully occupied, while those above are not. As temperature increases, thermal energy allows fermions to be excited to higher energy states, increasing the number of states partially occupied.
  • Influences quantum behaviors of particles.
  • Its value can shift the occupancy of fermionic states.
Understanding thermal energy helps explain why certain materials behave differently as they heat up or cool down, influencing properties like conductivity and magnetism.

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Most popular questions from this chapter

The heat capacity of liquid \(^{4} \mathrm{He}\) below \(0.6 \mathrm{K}\) is proportional to \(T^{3},\) with the measured value \(C_{V} / N k=(T / 4.67 \mathrm{K})^{3}\). This behavior suggests that the dominant excitations at low temperature are long-wavelength phonons. The only important difference between phonons in a liquid and phonons in a solid is that a liquid cannot transmit transversely polarized waves - sound waves must be longitudinal. The speed of sound in liquid \(^{4} \mathrm{He}\) is \(238 \mathrm{m} / \mathrm{s}\), and the density is \(0.145 \mathrm{g} / \mathrm{cm}^{3} .\) From these numbers, calculate the phonon contribution to the heat capacity of \(^{4} \mathrm{He}\) in the low-temperature limit, and compare to the measured value.

The Sommerfeld expansion is an expansion in powers of \(k T / \epsilon_{\mathrm{F}}\) which is assumed to be small. In this section I kept all terms through order \(\left(k T / \epsilon_{\mathrm{F}}\right)^{2},\) omitting higher-order terms. Show at each relevant step that the term proportional to \(T^{3}\) is zero, so that the next nonvanishing terms in the expansions for \(\mu\) and \(U\) are proportional to \(T^{4}\). (If you enjoy such things, you might try evaluating the \(T^{4}\) terms, possibly with the aid of a computer algebra program.)

Number of photons in a photon gas. (a) Show that the number of photons in equilibrium in a box of volume \(V\) at temperature \(T\) is $$N=8 \pi V\left(\frac{k T}{h c}\right)^{3} \int_{0}^{\infty} \frac{x^{2}}{e^{x}-1} d x$$ The integral cannot be done analytically; either look it up in a table or evaluate it numerically. (b) How does this result compare to the formula derived in the text for the entropy of a photon gas? (What is the entropy per photon, in terms of \(k ?\) ) (c) Calculate the number of photons per cubic meter at the following temperatures: 300 K; 1500 K (a typical kiln); 2.73 K (the cosmic background radiation).

Calculate the condensation temperature for liquid helium- 4 , pretending that the liquid is a gas of noninteracting atoms. Compare to the observed temperature of the superfluid transition, 2.17 K. (The density of liquid helium- 4 is \(0.145 \mathrm{g} / \mathrm{cm}^{3}\).)

At the center of the sun, the temperature is approximately \(10^{7} \mathrm{K}\) and the concentration of electrons is approximately \(10^{32}\) per cubic meter. Would it be (approximately) valid to treat these electrons as a "classical" ideal gas (using Boltzmann statistics), or as a degenerate Fermi gas (with \(T \approx 0\) ), or neither?

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