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In addition to the cosmic background radiation of photons, the universe is thought to be permeated with a background radiation of neutrinos (v) and antineutrinos (v-), currently at an effective temperature of 1.95 K. There are three species of neutrinos, each of which has an antiparticle, with only one allowed polarisation state for each particle or antiparticle. For parts (a) through (c) below, assume that all three species are exactly massless

(a) It is reasonable to assume that for each species, the concentration of neutrinos equals the concentration of antineutrinos, so that their chemical potentials are equal: =. Furthermore, neutrinos and antineutrinos can be produced and annihilated in pairs by the reaction

+2

(where y is a photon). Assuming that this reaction is at equilibrium (as it would have been in the very early universe), prove that u =0 for both the neutrinos and the antineutrinos.

(b) If neutrinos are massless, they must be highly relativistic. They are also fermions: They obey the exclusion principle. Use these facts to derive a formula for the total energy density (energy per unit volume) of the neutrino-antineutrino background radiation. differences between this "neutrino gas" and a photon gas. Antiparticles still have positive energy, so to include the antineutrinos all you need is a factor of 2. To account for the three species, just multiply by 3.) To evaluate the final integral, first change to a dimensionless variable and then use a computer or look it up in a table or consult Appendix B. (Hint: There are very few

(c) Derive a formula for the number of neutrinos per unit volume in the neutrino background radiation. Evaluate your result numerically for the present neutrino temperature of 1.95 K.

d) It is possible that neutrinos have very small, but nonzero, masses. This wouldn't have affected the production of neutrinos in the early universe, when me would have been negligible compared to typical thermal energies. But today, the total mass of all the background neutrinos could be significant. Suppose, then, that just one of the three species of neutrinos (and the corresponding antineutrino) has a nonzero mass m. What would mc2 have to be (in eV), in order for the total mass of neutrinos in the universe to be comparable to the total mass of ordinary matter?

Short Answer

Expert verified

Hence proved that v=v=0

Step by step solution

01

Given information

In addition to the cosmic background radiation of photons, the universe is thought to be permeated with a background radiation of neutrinos (v) and antineutrinos (v-), currently at an effective temperature of 1.95 K. There are three species of neutrinos, each of which has an antiparticle, with only one allowed polarisation state for each particle or antiparticle. For parts (a) through (c) below, assume that all three species are exactly massless.

02

Explanation

(a) In two pairs of photons, neutrinos and antineutrinos can be annihilated as follows:

v+v2

In terms of chemical potentials, the equilibrium condition for this reaction is:

v+v=2

Assume that the number of neutrinos in each species equals the number of antineutrinos, and that their chemical potentials are equal v=vand that the chemical potential of the photon is zero, as explained on page 290.

v=v=0

(b)The Fermi Dirac distribution, but with zero chemical potential, gives the likelihood of any single state being occupied by a neutrino:

nFD=1e/kT+1

The total energy equals the sum over the energies multiplied by their probabilities, that is:

U=32nxnynznFD

Now, factor 2 comes from the fact that anti matter (neutrinos and antineutrinos) exists, and factor 3 comes from the fact that we have three spices. Consider a cubic box with a volume of V and a side width of L. The permitted energy for neutrinos is:

=hcn2L

Hence,

U=6nx,ny,nze/kT+1U=6nx,ny,nzhcn/2Lehcn/2LkT+1

We must now convert the total to an integral in spherical coordinates, which we may do by multiplying it by the spherical integration factor n2sin()so:

U=60/2d0/2sin()d0(hc/2L)n3ehcn/2LkT+1dn

The first two integrals are easy to evaluate, and they give a factor of /2, so:

U=30(hc/2L)n3ehcn/2LkT+1dn

03

Calculation

Let,

x=hcn2LkTdx=hc2LkTdn

Hence,

U=32LkThc4hc2L0x3ex+1dxU=32Lhc3(kT)40x3ex+1dx

The integral is given as:

0x3ex+1dx=74120

Thus,

U=32Lhc3(kT)474120

Volume of box is V=L3

U=24V(kT)4(hc)374120UV=75(kT)45(hc)3

(c)The number of neutrinos can be computed in the same way as the number of protons, but without the factor , yielding:

N=60/2d0/2sin()d0(hc/2L)n3ehcn/2LkT+1dn

The first two integrals are easy to evaluate, and they give a factor of /2, so:

N=30n2ehcn/2LkT+1dn

Let,

x=hcn2LkTdx=hc2LkTdn

Thus,

N=32LkThc30x2ex+1dx

The value of the integral is 1.803, hence

N=3(1.803)2LkThc3

Volume of the box is V=L3

NV=24(1.803)kThc3NV=(135.94)kThc3

At temperature of 1 = 1.94 K, the number of neutrinos per unit volume is:

NV=(135.94)1.3810-23J/K(1.94K)6.62610-34Js3.0108m/s3NV=3.321108m-3

04

Explanation

(d)Assuming that there is only one type of neutrino, the number of neutrinos per unit volume is one-third of what we computed in the preceding section, i.e.

NV=1.1108m-3

The average density of the universe is one proton per cubic metre, and the energy of this proton in eV is mpc2=1.0109eV per cubic metre, hence the neutrino's energy should be:

mnc2=1.0109m-31.1108m-3mnc2=11eV

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Most popular questions from this chapter

Use the results of this section to estimate the contribution of conduction electrons to the heat capacity of one mole of copper at room temperature. How does this contribution compare to that of lattice vibrations, assuming that these are not frozen out? (The electronic contribution has been measured at low temperatures, and turns out to be about40% more than predicted by the free electron model used here.)

Consider a gas of noninteracting spin-0 bosons at high temperatures, when TTc. (Note that 鈥渉igh鈥 in this sense can still mean below 1 K.)

  1. Show that, in this limit, the Bose-Einstein function can be written approximately as
    nBE=e()/kT[1+e/kT+].
  2. Keeping only the terms shown above, plug this result into equation 7.122 to derive the first quantum correction to the chemical potential for gas of bosons.
  3. Use the properties of the grand free energy (Problems 5.23 and 7.7) to show that the pressure of any system is given by In P=(kT/V), where Zis the grand partition function. Argue that, for gas of noninteracting particles, In Zcan be computed as the sum over all modes (or single-particle states) of In Zi, where Zi; is the grand partition function for the ithmode.
  4. Continuing with the result of part (c), write the sum over modes as an integral over energy, using the density of states. Evaluate this integral explicitly for gas of noninteracting bosons in the high-temperature limit, using the result of part (b) for the chemical potential and expanding the logarithm as appropriate. When the smoke clears, you should find
    p=NkTV(1NvQ42V),
    again neglecting higher-order terms. Thus, quantum statistics results in a lowering of the pressure of a boson gas, as one might expect.
  5. Write the result of part (d) in the form of the virial expansion introduced in Problem 1.17, and read off the second virial coefficient, B(T). Plot the predicted B(T)for a hypothetical gas of noninteracting helium-4 atoms.
  6. Repeat this entire problem for gas of spin-1/2 fermions. (Very few modifications are necessary.) Discuss the results, and plot the predicted virial coefficient for a hypothetical gas of noninteracting helium-3 atoms.

Imagine that there exists a third type of particle, which can share a single-particle state with one other particle of the same type but no more. Thus the number of these particles in any state can be 0,1 or 2 . Derive the distribution function for the average occupancy of a state by particles of this type, and plot the occupancy as a function of the state's energy, for several different temperatures.

Carry out the Sommerfeld expansion for the energy integral (7.54), to obtain equation 7.67. Then plug in the expansion for to obtain the final answer, equation 7.68.

In this problem you will model helium-3 as a non-interacting Fermi gas. Although He3liquefies at low temperatures, the liquid has an unusually low density and behaves in many ways like a gas because the forces between the atoms are so weak. Helium-3 atoms are spin-1/2 fermions, because of the unpaired neutron in the nucleus.

(a) Pretending that liquid 3He is a non-interacting Fermi gas, calculate the Fermi energy and the Fermi temperature. The molar volume (at low pressures) is 37cm3

(b)Calculate the heat capacity for T<<Tf, and compare to the experimental result CV=(2.8K-1)NkT(in the low-temperature limit). (Don't expect perfect agreement.)

(c)The entropy of solid H3ebelow 1 K is almost entirely due to its multiplicity of nuclear spin alignments. Sketch a graph S vs. T for liquid and solid H3eat low temperature, and estimate the temperature at which the liquid and solid have the same entropy. Discuss the shape of the solid-liquid phase boundary shown in Figure 5.13.

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