Change variables in equation 7.83 to λ=hc/ϵ and thus derive a formula for the photon spectrum as a function of wavelength. Plot this spectrum, and find a numerical formula for the wavelength where the spectrum peaks, in terms of hc/kT. Explain why the peak does not occur at hc/(2.82kT).

Short Answer

Expert verified

Hence, formula for the photon spectrum as a function of wavelength isu(l)=8π(kT)4(hc)31l51e1/l-1

Step by step solution

01

Given information

Changing variables in equation 7.83 to λ=hc/ϵ and thus deriving a formula for the photon spectrum as a function of wavelength.

02

Explanation

The equation 7.83 is:

UV=8π(hc)30ϵ3eϵ/kT-1dϵ(1)

Change the variables to the wavelength using,

ϵ=hcλdϵ=-hcλ2dλ

Substitute this into (1)

UV=-8π(hc)30(hc)4λ51ehc/kTλ-1dλ

03

Calculations

By changing the integration boundaries, at ϵ=0the wavelength isand atϵ=the wavelength is zero.

localid="1647752119716">UV=8πhc01λ51ehc/kTλ-1dλUV=8πhc01λ51ehc/kTλ-1dλ

Changing the function to be dimensionless variables,

l=kThcλ

Hence,

UV=8π(kT)4(hc)301l51e1/l-1dλ

u(l)=8π(kT)4(hc)31l51e1/l-1

Using python to solve this function. The code is:

The graph is:

The peak occurs at l=0.2014

0.2014=kThcλλ=0.2014hckTλ=hc4.965kT

This isn't the same as the solution to problem 7.37. This is due to the nonlinear relationship between energy and wavelength; for example, the energy difference between 1 eV and 2 eV is the same for 101 eV and 102 eV, but the wavelengths that correspond to these two intervals are not.

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Most popular questions from this chapter

The tungsten filament of an incandescent light bulb has a temperature of approximately 3000K. The emissivity of tungsten is approximately 13, and you may assume that it is independent of wavelength.

(a) If the bulb gives off a total of 100watts, what is the surface area of its filament in square millimetres?

(b) At what value of the photon energy does the peak in the bulb's spectrum occur? What is the wavelength corresponding to this photon energy?

(c) Sketch (or use a computer to plot) the spectrum of light given off by the filament. Indicate the region on the graph that corresponds to visible wavelengths, between400and700nm.

(d) Calculate the fraction of the bulb's energy that comes out as visible light. (Do the integral numerically on a calculator or computer.) Check your result qualitatively from the graph of part (c).

( e) To increase the efficiency of an incandescent bulb, would you want to raise or lower the temperature? (Some incandescent bulbs do attain slightly higher efficiency by using a different temperature.)

(f) Estimate the maximum possible efficiency (i.e., fraction of energy in the visible spectrum) of an incandescent bulb, and the corresponding filament temperature. Neglect the fact that tungsten melts at 3695K.

The speed of sound in copper is 3560m/s. Use this value to calculate its theoretical Debye temperature. Then determine the experimental Debye temperature from Figure 7.28, and compare.

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=8πVkThc30x2ex-1dx

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 condensate temperature for liquid helium-4, pretending that liquid is a gas of noninteracting atoms. Compare to the observed temperature of the superfluid transition, 2.17K. ( the density of liquid helium-4 is 0.145g/cm3)

For a brief time in the early universe, the temperature was hot enough to produce large numbers of electron-positron pairs. These pairs then constituted a third type of "background radiation," in addition to the photons and neutrinos (see Figure 7.21). Like neutrinos, electrons and positrons are fermions. Unlike neutrinos, electrons and positrons are known to be massive (ea.ch with the same mass), and each has two independent polarization states. During the time period of interest, the densities of electrons and positrons were approximately equal, so it is a good approximation to set the chemical potentials equal to zero as in Figure 7.21. When the temperature was greater than the electron mass times c2k, the universe was filled with three types of radiation: electrons and positrons (solid arrows); neutrinos (dashed); and photons (wavy). Bathed in this radiation were a few protons and neutrons, roughly one for every billion radiation particles. the previous problem. Recall from special relativity that the energy of a massive particle is ϵ=(pc)2+mc22.

(a) Show that the energy density of electrons and positrons at temperature Tis given by

u(T)=0x2x2+mc2/kT2ex2+mc2/kT2+1dx;whereu(T)=0x2x2+mc2/kT2ex2+mc2/kT2+1dx

(b) Show that u(T)goes to zero when kTmc2, and explain why this is a

reasonable result.

( c) Evaluate u(T)in the limit kTmc2, and compare to the result of the

the previous problem for the neutrino radiation.

(d) Use a computer to calculate and plot u(T)at intermediate temperatures.

(e) Use the method of Problem 7.46, part (d), to show that the free energy

density of the electron-positron radiation is

FV=-16π(kT)4(hc)3f(T);wheref(T)=0x2ln1+e-x2+mc2/kT2dx

Evaluate f(T)in both limits, and use a computer to calculate and plot f(T)at intermediate

temperatures.

(f) Write the entropy of the electron-positron radiation in terms of the functions

uTand f(T). Evaluate the entropy explicitly in the high-T limit.

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