(a)Use Equation5.113 to determine the energy density in the wavelength rangedλ. Hint: setρ(ω)=ρ-(λ), and solve forρ(λ)-

(b)Derive the Wien displacement law for the wavelength at which the blackbody energy density is a maximum
λmax=2.90×10-3mKT

You'll need to solve the transcendental equation(5×x)=5e-x, using a calculator (or a computer); get the numerical answer accurate to three significant digits.

Short Answer

Expert verified

aρ-λ=16π2hcλ5e2hc/ke-1bλmax=2.90×10-3mKT

Step by step solution

01

Given

The energy density in wavelength range is given by:

ρω=ρ-λ

02

Determining the energy density in the wavelength rangedλ

ω=2πc=2πcλ,so=-2πcλ2,andρω=hπ2c32πc3λ3e2πhc/kB-1ρω=8πh1λ3e2πhc/kB-1-2πcλ2=ρ-λρλ=16π2hcλ3e2πhc/kB-1-

For density we want only the size of the interval, not its sign)

03

Deriving the Wien displacement law for wavelength

To find maximize, we need to calculate:

dρ-/=0;0=16π2hc5λ6e2πhc/kB-1-e2πhc/kB2πhc/kBTλ6e2πhc/kB-12-1λ2A=2πhckBT5=AλeA/γeA/γ-15e-A/λ=5-Aλ

Using mathematicAλ=4.966

λmax=A4.966=2πhc4.966kBTλmax=2.90×10-3mKT

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Most popular questions from this chapter

Show that most of the energies determined by Equation 5.64are doubly degenerate. What are the exceptional cases? Hint: Try it for N=1,2,3,4.... , to see how it goes. What are the possible values of cos(ka)in each case?

Suppose you had three particles, one in stateψa(x), one in stateψb(x), and one in stateψc(x). Assuming ψa,ψb, andψc are orthonormal, construct the three-particle states (analogous to Equations 5.15,5.16, and 5.17) representing

(a) distinguishable particles,

(b) identical bosons, and

(c) identical fermions.

Keep in mind that (b) must be completely symmetric, under interchange of any pair of particles, and (c) must be completely antisymmetric, in the same sense. Comment: There's a cute trick for constructing completely antisymmetric wave functions: Form the Slater determinant, whose first row isψa(x1),ψb(x1),ψc(x1) , etc., whese second row isψa(x2),ψb(x2),ψc(x2) , etc., and so on (this device works for any number of particles).

We can extend the theory of a free electron gas (Section 5.3.1) to the relativistic domain by replacing the classical kinetic energy, E=p2/2m,,with the relativistic formula, E=p2c2+m2c4-mc2. Momentum is related to the wave vector in the usual way: p=hk. In particular, in the extreme relativistic limit, Epc=hck.

(a) Replace h2k2n Equation 5.55 by the ultra-relativistic expression, hck, and calculateEtotin this regime.

dE=h2k22mVπ2k2dk (5.55).

(b) Repeat parts (a) and (b) of Problem 5.35 for the ultra-relativistic electron gas. Notice that in this case there is no stable minimum, regardless of R; if the total energy is positive, degeneracy forces exceed gravitational forces, and the star will expand, whereas if the total is negative, gravitational forces win out, and the star will collapse. Find the critical number of nucleons, Nc , such that gravitational collapse occurs for N>N_{C}is called the Chandrasekhar limit.

(c) At extremely high density, inverse beta decaye-+p+n+v,converts virtually all of the protons and electrons into neutrons (liberating neutrinos, which carry off energy, in the process). Eventually neutron degeneracy pressure stabilizes the collapse, just as electron degeneracy does for the white dwarf (see Problem 5.35). Calculate the radius of a neutron star with the mass of the sun. Also calculate the (neutron) Fermi energy, and compare it to the rest energy of a neutron. Is it reasonable to treat a neutron star non relativistic ally?

Derive the Stefan-Boltzmann formula for the total energy density in blackbody radiation

EV=(π2kB415ħ3C3)T4=7.57×10-16Jm-3K-4T4

The ground state of dysprosium (element 66, in the 6th row of the Periodic Table)

is listed as Is5. What are the total spin, total orbital, and grand total angular

momentum quantum numbers? Suggest a likely electron configuration for

dysprosium.

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