Chapter 7: Q. 7.65 (page 323)
Evaluate the integral in equation numerically, to confirm the value quoted in the text.
Short Answer
The integral in equationis evaluated in simpler form.
Chapter 7: Q. 7.65 (page 323)
Evaluate the integral in equation numerically, to confirm the value quoted in the text.
The integral in equationis evaluated in simpler form.
All the tools & learning materials you need for study success - in one app.
Get started for freeFill in the steps to derive equations and.
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 , 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 .
(a) Show that the energy density of electrons and positrons at temperature is given by
(b) Show that goes to zero when , and explain why this is a
reasonable result.
( c) Evaluate in the limit , and compare to the result of the
the previous problem for the neutrino radiation.
(d) Use a computer to calculate and plot 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
Evaluate in both limits, and use a computer to calculate and plot at intermediate
temperatures.
(f) Write the entropy of the electron-positron radiation in terms of the functions
and . Evaluate the entropy explicitly in the high-T limit.
Sketch the heat capacity of copper as a function of temperature from to, showing the contributions of lattice vibrations and conduction electrons separately. At what temperature are these two contributions equal?
Compute the quantum volume for an molecule at room temperature, and argue that a gas of such molecules at atmospheric pressure can be
treated using Boltzmann statistics. At about what temperature would quantum statistics become relevant for this system (keeping the density constant and pretending that the gas does not liquefy)?
Change variables in equation 7.83 to 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).
What do you think about this solution?
We value your feedback to improve our textbook solutions.