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Consider the electromagnetic radiation inside a kiln, with a volume of V= I m3 and a temperature of 1500 K.

(a) What is the total energy of this radiation?

(b) Sketch the spectrum of the radiation as a function of photon energy.

(c) What fraction of all the energy is in the visible portion of the spectrum, with wavelengths between 400 nm and 700 nm?

Short Answer

Expert verified

Therefore, the total energy of this radiation is:

U=3.815×10-3J

Fraction of all energy isUvis.Utot.=0.000557

Step by step solution

01

Given information

The electromagnetic radiation inside a kiln, with a volume of V=I m3 and a temperature of 1500 K.

02

Explanation

(a) Suppose we have an electromagnetic radiation inside a kiln, which has a volume of V = 1 m3 and temperature of T = 1500 K, the total energy of this radiation is given by:

U=8π5(kT)415(hc)3V

Substitute with the values,

U=8π51.38×10-23J/K(1500K)4156.626×10-34J·s3.0×108m/s31m3U=3.815×10-3J

(b) The radiation's spectrum is provided by:

u(ϵ)=8π(hc)3ϵ3eϵ/kT-1

Using python and the code is:

From the graph we can see that the peak occurs at energy of ϵ=0.36eV

03

Explanation

(c) Now we need to discover the component of the spectrum that represents visible light (the fraction of the energy), which we can do by integrating the following equation all across the visible light (equation 785):

U=8πV(hc)3ϵ1ϵ2x3ex-1dx

The energy in terms of wavelength is:

ϵ=hcλ

Therefore,

ϵ2=6.626×10-34J·s3.0×108m/s400×10-9m=4.9695×10-19J=3.1eVϵ1=6.626×10-34J·s3.0×108m/s700×10-9m=2.84×10-19J=1.77eV

The fraction of the energy in the visible light is given by:

Uvis.Utot.=1.77eV3.1eVx3ex-1dx0x3ex-1dx

The integration in the denominator equals π4/15, therefore

Uvis.Utot=15π41.77eV3.1eVx3ex-1dϵ

But this is not the real boundaries since the integration over x not ϵ, we have:

x=ϵkT

But temperature T=1500K

localid="1647756536663">x1=ϵ1kT=1.77eV8.62×10-5eV/K(1500K)=13.7x2=ϵ2kT=3.1eVeV8.62×10-5eV/K(1500K)=24

Therefore, the integral will be:

Uvis.Utot.=15π413.724x3ex-1dϵ

To solve this integral python is used, the code is and the ratio is:

Uvis.Utot.=0.000557

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Most popular questions from this chapter

Consider a Bose gas confined in an isotropic harmonic trap, as in the previous problem. For this system, because the energy level structure is much simpler than that of a three-dimensional box, it is feasible to carry out the sum in equation 7.121 numerically, without approximating it as an integral.*

(a) Write equation 7.121 for this system as a sum over energy levels, taking degeneracy into account. Replace Tandμwith the dimensionless variables t=kT/hfandc=μ/hf.

(b) Program a computer to calculate this sum for any given values of tandc. Show that, for N=2000, equation 7.121 is satisfied at t=15provided that c=-10.534. (Hint: You'll need to include approximately the first 200 energy levels in the sum.)

(c) For the same parameters as in part (b), plot the number of particles in each energy level as a function of energy.

(d) Now reduce tto 14 , and adjust the value of cuntil the sum again equals 2000. Plot the number of particles as a function of energy.

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In Section 6.5 I derived the useful relation F=-kTln(Z)between the Helmholtz free energy and the ordinary partition function. Use analogous argument to prove that ϕ=-kT×ln(Z^), where Z^ is the grand partition function and ϕis the grand free energy introduced in Problem 5.23.

A star that is too heavy to stabilize as a white dwarf can collapse further to form a neutron star: a star made entirely of neutrons, supported against gravitational collapse by degenerate neutron pressure. Repeat the steps of the previous problem for a neutron star, to determine the following: the mass radius relation; the radius, density, Fermi energy, and Fermi temperature of a one-solar-mass neutron star; and the critical mass above which a neutron star becomes relativistic and hence unstable to further collapse.

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.*

Consider any two internal states, s1 and s2, of an atom. Let s2 be the higher-energy state, so that Es2-Es1=ϵ for some positive constant. If the atom is currently in state s2, then there is a certain probability per unit time for it to spontaneously decay down to state s1, emitting a photon with energy e. This probability per unit time is called the Einstein A coefficient:

A = probability of spontaneous decay per unit time.

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B=probability of absorption per unit timeu(f)

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B'=probability of stimulated emission per unit timeu(f)

As Einstein showed in 1917, knowing any one of these three coefficients is as good as knowing them all.

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