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In the text I claimed that the universe was filled with ionised gas until its temperature cooled to about 3000 K. To see why, assume that the universe contains only photons and hydrogen atoms, with a constant ratio of 109 photons per hydrogen atom. Calculate and plot the fraction of atoms that were ionised as a function of temperature, for temperatures between 0 and 6000 K. How does the result change if the ratio of photons to atoms is 108 or 1010? (Hint: Write everything in terms of dimensionless variables such as t = kT/I, where I is the ionisation energy of hydrogen.)

Short Answer

Expert verified

The fraction of atoms that were ionised as a function of temperature isf=-1+1+45.245×10-7(α)t3/2e1/t25.245×10-7(α)t3/2e1/t

Step by step solution

01

Given information

The universe was filled with ionised gas until its temperature cooled to about 3000K.

Assume that the universe contains only photons and hydrogen atoms, with a constant ratio of 109 photons per hydrogen atom.

02

Explanation

If f is the fraction of atoms that are ionised, then the proportion of ionised to non-ionised atoms is:

f=NpNp+NH(1)

Where Np is number of protons and these are ionised hydrogen.

The equation is:

NpNeNH=VvQe-I/kT

For each proton there is an electron so Ne=Np, hence the equation becomes:

Np2NH=VvQe-I/kT(2)

The number of photographs multiplied by a factor (say α) equals the number of ionised hydrogen atoms plus the number of un-ionised hydrogen atoms:

Np+NH=αNγ

Where Nγis the number of photons and is given by:

Nγ=8π(2.404)VkThc3

Thus,

Np+NH=αbVkThc3(3)

Substitute into (1)

Np=fNp+NHNp=fαbVkThc3(4)

Substitute int (3):

fαbVkThc3+NH=αbVkThc3NH=(1-f)αbVkThc3

Substitute from (5) and (4) into (2):

fαbVkThc32(1-f)αbVkThc3=VvQe-I/kTfαbkThc3(1-f)=1vQe-I/kTf2αbkThc3vQeI/kT=1-f(6)

Let

β=αbkThc3vQeI/kTwherevQ=h22πmkT3/2β=αbkT2πmc23/2eI/kT

Therefore,

βf2=1-fβf2+f-1=0

This is a quadratic equation.

03

Explanation:

The solution for quadratic equation is:

f=-1+1+4β2β(7)

Since we need to plot this equation, we need to change the variables into dimensionless variables, substituting the values

t=kTI

Then

β=αbIt2πmc23/2e1/tβ=αbI2πmc23/2t3/2e1/t

Substitute the given values to find the constant:

β=8π(2.404)(α)13.6×1.6×10-19J2π9.11×10-31kg3.0×108m/s23/2t3/2e1/tβ=5.245×10-7(α)t3/2e1/t

Substitute into (7)

f=-1+1+45.245×10-7(α)t3/2e1/t25.245×10-7(α)t3/2e1/t

This formula can be plot first forα=10-9then for10-8and10-10on same graph using python. The code is:

The graph is:

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Most popular questions from this chapter

Problem 7.67. In the first achievement of Bose-Einstein condensation with atomic hydrogen, a gas of approximately 2×1010atoms was trapped and cooled until its peak density was1.8×1014atoms/cm3. Calculate the condensation temperature for this system, and compare to the measured value of50μK.

Consider two single-particle states, A and B, in a system of fermions, where ϵA=μ-xand ϵB=μ+x; that is, level A lies below μ by the same amount that level B lies above μ. 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 ϵ=μ.

Compute the quantum volume for an N2molecule 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)?

The results of the previous problem can be used to explain why the current temperature of the cosmic neutrino background (Problem 7.48) is 1.95 K rather than 2.73 K. Originally the temperatures of the photons and the neutrinos would have been equal, but as the universe expanded and cooled, the interactions of neutrinos with other particles soon became negligibly weak. Shortly thereafter, the temperature dropped to the point where kT/c2 was no longer much greater than the electron mass. As the electrons and positrons disappeared during the next few minutes, they "heated" the photon radiation but not the neutrino radiation.

(a) Imagine that the universe has some finite total volume V, but that V is increasing with time. Write down a formula for the total entropy of the electrons, positrons, and photons as a function of V and T, using the auxiliary functions u(T) and f(T) introduced in the previous problem. Argue that this total entropy would have ben conserved in the early universe, assuming that no other species of particles interacted with these.

(b) The entropy of the neutrino radiation would have been separately conserved during this time period, because the neutrinos were unable to interact with anything. Use this fact to show that the neutrino temperature Tv and the photon temperature T are related by

TTν32π445+u(T)+f(T)=constant

as the universe expands and cools. Evaluate the constant by assuming that T=Tv when the temperatures are very high.

(c) Calculate the ratio T/Tv, in the limit of low temperature, to confirm that the present neutrino temperature should be 1.95 K.

(d) Use a computer to plot the ratio T/Tv, as a function of T, for kT/mc2ranging from 0 to 3.*

At the surface of the sun, the temperature is approximately 5800 K.

(a) How much energy is contained in the electromagnetic radiation filling a cubic meter of space at the sun's surface?

(b) Sketch the spectrum of this radiation as a function of photon energy. Mark the region of the spectrum that corresponds to visible wavelengths, between 400 nm and 700 nm.

(c) What fraction of the energy is in the visible portion of the spectrum? (Hint: Do the integral numerically.)

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