Waves and Modern Physics 203-SN3-RE • CEGEP, Montreal

Corrected exercises: quantum physics, photons, line spectra and duality (203-SN3-RE)

This is a set of fifteen corrected exercises on quantum physics for element 3 of Waves and Modern Physics, 203-SN3-RE (formerly 203-NYC), in the revised Natural Science program (200.B1): the photon, blackbody radiation, the Bohr model, wave-particle duality and line spectra. It builds on the overview set on modern physics without repeating any of its exercises, so that the quantum block gets the depth of a full chapter.

Part A lays out the objects: the photon as a carrier of momentum, the lines of hydrogen through the Rydberg formula, Bohr orbits read as standing waves, one-electron ions and the diffraction of electrons. Part B confronts them with the experiments on which the theory was founded: X-rays, Franck and Hertz, spectral shift, photon counting. Part C goes through the classics of the chapter, from the particle in a box to the natural width of a spectral line.

The thread of the set: at the scale of the atom, energy is exchanged only in packets, and it is the WAVE condition that fixes those packets. A bound electron is a standing wave, like a vibrating string; only certain wavelengths fit, so only certain energies exist. Nearly every mistake in the chapter comes from confusing intensity with energy, or from leaving a wavelength in nanometres in a formula that expects metres.

15 corrected exercises • 150 points • 225 minutes

This chapter is part of 203-SN3-RE, every chapter with its set and sheet Before you start Revision sheet: the traps and the method for this chapter

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Course recap

  • • Photon: E=hf=hcλE=hf=\dfrac{hc}{\lambda}, p=hλ=Ecp=\dfrac{h}{\lambda}=\dfrac{E}{c}. Shortcut: E(eV)=1240λ(nm)E(\mathrm{eV})=\dfrac{1240}{\lambda(\mathrm{nm})}.
  • • Rydberg formula: 1λ=RH(1n12−1n22)\dfrac{1}{\lambda}=R_{H}\left(\dfrac{1}{n_{1}^{2}}-\dfrac{1}{n_{2}^{2}}\right), RH=1.097×107R_{H}=1.097\times 10^{7} m⁻¹; Lyman n1=1n_{1}=1 (UV), Balmer n1=2n_{1}=2 (visible), Paschen n1=3n_{1}=3 (IR).
  • • Bohr model: mevr=nℏm_{e}vr=n\hbar, rn=n2Za0r_{n}=\dfrac{n^{2}}{Z}a_{0} with a0=0.0529a_{0}=0.0529 nm, En=−13.6 Z2n2E_{n}=-\dfrac{13.6\,Z^{2}}{n^{2}} eV.
  • • de Broglie wavelength: λ=hp\lambda=\dfrac{h}{p}; electron accelerated through VV: λ=h2meeV\lambda=\dfrac{h}{\sqrt{2m_{e}eV}}.
  • • Particle in a box of width LL: En=n2h28mL2E_{n}=\dfrac{n^{2}h^{2}}{8mL^{2}}, n≥1n\ge 1.
  • • X-rays: λmin=hceV\lambda_{min}=\dfrac{hc}{eV}; Moseley's law EKα≈10.2 (Z−1)2E_{K\alpha}\approx 10.2\,(Z-1)^{2} eV.
  • • Boltzmann: N2N1=g2g1e−ΔE/(kT)\dfrac{N_{2}}{N_{1}}=\dfrac{g_{2}}{g_{1}}e^{-\Delta E/(kT)}, k=8.62×10−5k=8.62\times 10^{-5} eV/K.
  • • Energy-time uncertainty: ΔE Δt≈ℏ\Delta E\,\Delta t\approx\hbar; natural linewidth Δf=12πτ\Delta f=\dfrac{1}{2\pi\tau}.

Part A: the basics (/50)

Exercise 1: The momentum of the photon: the solar sail

A photon of wavelength λ\lambda carries a momentum p=hλp=\dfrac{h}{\lambda}, even though it has no mass. A perfectly reflecting solar sail of 100100 m², facing the Sun at the distance of the Earth, receives a flux of 13611361 W/m². The probe has a total mass of 10.010.0 kg. Take a mean wavelength of 550550 nm.

Constants: h=6.63×10−34h=6.63\times 10^{-34} J·s, c=3.00×108c=3.00\times 10^{8} m/s, e=1.60×10−19e=1.60\times 10^{-19} C, me=9.11×10−31m_{e}=9.11\times 10^{-31} kg, hc=1240hc=1240 eV·nm. The diagram below shows the situation.

Sunincident photon, 550 nmreflected photonreflective sail100 m², 1361 W/m²probe: 10.0 kg
  • a) Calculate the momentum of a 550550 nm photon.
  • b) Calculate the number of photons striking the sail each second.
  • c) A reflected photon leaves in the opposite direction. What momentum does it transfer to the sail, in terms of pp?
  • d) Show that the force is F=2IAcF=\dfrac{2IA}{c} and calculate it.
  • e) Calculate the speed gained by the probe in one day, starting from rest.

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  • a) p=1.21×10−27p=1.21\times 10^{-27} kg·m/s
  • b) N=3.76×1023N=3.76\times 10^{23} photons/s
  • c) 2p2p
  • d) F=9.07×10−4F=9.07\times 10^{-4} N
  • e) v≈7.84v\approx 7.84 m/s
a)

p=hλ=6.63×10−34550×10−9=1.21×10−27p=\dfrac{h}{\lambda}=\dfrac{6.63\times 10^{-34}}{550\times 10^{-9}}=1.21\times 10^{-27} kg·m/s.

b)

Power received: P=IA=1361×100=1.36×105P=IA=1361\times 100=1.36\times 10^{5} W. Energy of one photon: E=hcλ=3.62×10−19E=\dfrac{hc}{\lambda}=3.62\times 10^{-19} J. Number per second: N=PE=3.76×1023N=\dfrac{P}{E}=3.76\times 10^{23} photons/s.

c)

The momentum goes from +p+p to −p-p: its change is −2p-2p, and the sail receives +2p+2p. An absorbing sail would receive only pp: reflecting doubles the thrust, exactly as a bouncing ball transfers more impulse than a ball that sticks.

d)

F=N×2p=IAE×2Ec=2IAcF=N\times 2p=\dfrac{IA}{E}\times\dfrac{2E}{c}=\dfrac{2IA}{c}, since p=Ecp=\dfrac{E}{c} for a photon. The wavelength drops out of the result. F=2×1361×1003.00×108=9.07×10−4F=\dfrac{2\times 1361\times 100}{3.00\times 10^{8}}=9.07\times 10^{-4} N, the weight of a tenth of a gram.

e)

a=Fm=9.07×10−5a=\dfrac{F}{m}=9.07\times 10^{-5} m/s², and over 86 40086\,400 s: v=at=7.84v=at=7.84 m/s. That is negligible after one day, but the thrust never stops and uses no fuel: after one year, 2.92.9 km/s.

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Exercise 2: The Rydberg formula and the Balmer series

The wavelengths of the lines of hydrogen obey the Rydberg formula: 1λ=RH(1n12−1n22)\dfrac{1}{\lambda}=R_{H}\left(\dfrac{1}{n_{1}^{2}}-\dfrac{1}{n_{2}^{2}}\right) with n2>n1n_{2}>n_{1} and RH=1.097×107R_{H}=1.097\times 10^{7} m⁻¹. The Balmer series, which is visible, corresponds to n1=2n_{1}=2. The spectrum below shows four of its lines.

350400450500550600650700λ (nm)410434486?
  • a) Calculate the wavelength of the line n2=3→n1=2n_{2}=3\rightarrow n_{1}=2.
  • b) Which transition produces the line at 410410 nm? Give n2n_{2}.
  • c) Calculate the limit of the Balmer series (n2→∞n_{2}\to\infty).
  • d) Calculate the wavelength of the first line of the Lyman series (n1=1n_{1}=1, n2=2n_{2}=2). In which region is it?
  • e) Why do the Balmer lines crowd together toward the short wavelengths?

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  • a) 656656 nm (Hα\alpha)
  • b) 6→26\rightarrow 2
  • c) λlim=365\lambda_{lim}=365 nm
  • d) 122122 nm, ultraviolet
  • e) Levels in −1/n2-1/n^{2} that crowd together
a)

1λ=1.097×107(14−19)=1.524×106\dfrac{1}{\lambda}=1.097\times 10^{7}\left(\dfrac{1}{4}-\dfrac{1}{9}\right)=1.524\times 10^{6} m⁻¹, so λ=656\lambda=656 nm: the red line Hα\alpha.

b)

Try successive values: n2=4n_{2}=4 gives 486486 nm, n2=5n_{2}=5 gives 434434 nm, n2=6n_{2}=6 gives 11.097×107(1/4−1/36)=410\dfrac{1}{1.097\times 10^{7}(1/4-1/36)}=410 nm. It is the transition 6→26\rightarrow 2.

c)

When n2→∞n_{2}\to\infty, 1n22→0\dfrac{1}{n_{2}^{2}}\to 0: λlim=4RH=3.65×10−7\lambda_{lim}=\dfrac{4}{R_{H}}=3.65\times 10^{-7} m =365=365 nm, in the near ultraviolet. No Balmer line has a shorter wavelength.

d)

1λ=1.097×107×34\dfrac{1}{\lambda}=1.097\times 10^{7}\times\dfrac{3}{4}, so λ=122\lambda=122 nm, in the far ULTRAVIOLET. The whole Lyman series is invisible and absorbed by the atmosphere: it is observed from space.

e)

The energy levels, which go as −1n2-\dfrac{1}{n^{2}}, get closer together as nn increases. The gaps from level 22 therefore tend toward a limiting value: the emitted photons have energies that get closer and closer, and the lines pile up near the limit of 365365 nm.

Exercise 3: The Bohr model: radii, speeds and the standing wave

In the Bohr model, the electron of hydrogen follows circular orbits on which its angular momentum is quantized: mevr=nℏm_{e}vr=n\hbar. It follows that rn=n2a0r_{n}=n^{2}a_{0} with a0=0.0529a_{0}=0.0529 nm, and vn=v1nv_{n}=\dfrac{v_{1}}{n} with v1=2.19×106v_{1}=2.19\times 10^{6} m/s.

Constants: h=6.63×10−34h=6.63\times 10^{-34} J·s, c=3.00×108c=3.00\times 10^{8} m/s, e=1.60×10−19e=1.60\times 10^{-19} C, me=9.11×10−31m_{e}=9.11\times 10^{-31} kg, hc=1240hc=1240 eV·nm. The diagram below shows the model.

+protonrelectronvcircular orbit, m v r = n ħ
  • a) Calculate the radius of the orbit n=3n=3.
  • b) Calculate the speed of the electron on this orbit.
  • c) Calculate the period of revolution of the electron on the orbit n=1n=1.
  • d) Calculate the de Broglie wavelength of the electron on the orbit n=1n=1 and compare it with the circumference 2πa02\pi a_{0}.
  • e) “Rydberg” atoms are prepared in the state n=100n=100. What is their radius, in µm?

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  • a) r3=0.476r_{3}=0.476 nm
  • b) v3=7.30×105v_{3}=7.30\times 10^{5} m/s
  • c) T=1.52×10−16T=1.52\times 10^{-16} s
  • d) λ=3.32×10−10\lambda=3.32\times 10^{-10} m =2πa0=2\pi a_{0}
  • e) r100=0.529r_{100}=0.529 µm
a)

r3=9×0.0529=0.476r_{3}=9\times 0.0529=0.476 nm.

b)

v3=2.19×1063=7.30×105v_{3}=\dfrac{2.19\times 10^{6}}{3}=7.30\times 10^{5} m/s.

c)

T=2πa0v1=2π×5.29×10−112.19×106=1.52×10−16T=\dfrac{2\pi a_{0}}{v_{1}}=\dfrac{2\pi\times 5.29\times 10^{-11}}{2.19\times 10^{6}}=1.52\times 10^{-16} s. That is a frequency of 6.6×10156.6\times 10^{15} Hz, of the same order as that of ultraviolet light: this is what made the model plausible.

d)

λ=hmev1=6.63×10−349.11×10−31×2.19×106=3.32×10−10\lambda=\dfrac{h}{m_{e}v_{1}}=\dfrac{6.63\times 10^{-34}}{9.11\times 10^{-31}\times 2.19\times 10^{6}}=3.32\times 10^{-10} m, and 2πa0=3.32×10−102\pi a_{0}=3.32\times 10^{-10} m. They are equal: the ground-state orbit contains exactly ONE wavelength. In general 2πrn=nλn2\pi r_{n}=n\lambda_{n} is the Bohr condition rewritten, since mevr=nℏm_{e}vr=n\hbar is equivalent to 2πr=nhmev2\pi r=n\dfrac{h}{m_{e}v}: the electron is a standing wave that closes on itself, like a vibrating string bent into a ring.

e)

r100=104×0.0529r_{100}=10^{4}\times 0.0529 nm =529=529 nm =0.529=0.529 µm, ten thousand times the size of an ordinary atom, almost the size of a bacterium. These giant atoms, very sensitive to electric fields, are used today in quantum optics.

Exercise 4: Hydrogen-like ions: when the charge of the nucleus changes everything

A hydrogen-like ion has a nucleus of charge +Ze+Ze and a single electron: He⁺ (Z=2Z=2), Li²⁺ (Z=3Z=3). The Bohr model applies to it with En=−13.6 Z2n2E_{n}=-\dfrac{13.6\,Z^{2}}{n^{2}} eV and rn=n2Za0r_{n}=\dfrac{n^{2}}{Z}a_{0}. Take hc=1240hc=1240 eV·nm.

  • a) Calculate the ionization energy of He⁺ from its ground state.
  • b) Same question for Li²⁺.
  • c) Calculate the energy of the photon emitted by He⁺ in the transition 4→34\rightarrow 3.
  • d) Calculate its wavelength. In which region is it?
  • e) By what factor is the radius of the ground-state orbit of Li²⁺ smaller than that of hydrogen?

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  • a) 54.454.4 eV
  • b) 122.4122.4 eV
  • c) ΔE=2.64\Delta E=2.64 eV
  • d) λ=469\lambda=469 nm, blue
  • e) Three times smaller
a)

Eion=13.6×22=54.4E_{ion}=13.6\times 2^{2}=54.4 eV. The electron is attracted by a double charge, at half the distance: it is bound four times as strongly.

b)

Eion=13.6×9=122.4E_{ion}=13.6\times 9=122.4 eV.

c)

ΔE=54.4(19−116)=54.4×7144=2.64\Delta E=54.4\left(\dfrac{1}{9}-\dfrac{1}{16}\right)=54.4\times\dfrac{7}{144}=2.64 eV.

d)

λ=12402.644=469\lambda=\dfrac{1240}{2.644}=469 nm, in the BLUE. This line of ionized helium, observed in the Sun and in hot stars, was at first wrongly attributed to hydrogen. Note: 4→34\rightarrow 3 belongs to no visible series of hydrogen; it is the factor Z2=4Z^{2}=4 that brings the line back into the visible.

e)

r1=a0Zr_{1}=\dfrac{a_{0}}{Z}: three times smaller. The energy, for its part, is multiplied by Z2=9Z^{2}=9: the two effects, a stronger charge and a shorter distance, combine.

Exercise 5: Electron diffraction: the Davisson and Germer experiment

In 1927, Davisson and Germer sent electrons accelerated through 5454 V onto a nickel crystal whose surface rows of atoms are spaced d=0.215d=0.215 nm apart. They observed a maximum of scattering in a direction θ\theta such that dsin⁡θ=λd\sin\theta=\lambda, as for a grating.

Constants: h=6.63×10−34h=6.63\times 10^{-34} J·s, c=3.00×108c=3.00\times 10^{8} m/s, e=1.60×10−19e=1.60\times 10^{-19} C, me=9.11×10−31m_{e}=9.11\times 10^{-31} kg, hc=1240hc=1240 eV·nm. Mass of the neutron 1.675×10−271.675\times 10^{-27} kg. The diagram below shows the experiment.

nickel crystald = 0.215 nmelectron gunaccelerated through 54 Velectronsθdetector
  • a) Show that the de Broglie wavelength of an electron accelerated through VV is λ=h2meeV\lambda=\dfrac{h}{\sqrt{2m_{e}eV}} and calculate it for V=54V=54 V.
  • b) Calculate the angle θ\theta of the scattering maximum.
  • c) Through what voltage would the electrons have to be accelerated to halve their wavelength?
  • d) “Thermal” neutrons have a kinetic energy of 0.0250.025 eV. Calculate their wavelength.
  • e) Why are electrons and thermal neutrons suited to studying crystals, but visible light is not?

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  • a) λ=0.167\lambda=0.167 nm
  • b) θ≈51°\theta\approx 51°
  • c) V=216V=216 V
  • d) λ=0.181\lambda=0.181 nm
  • e) λ\lambda comparable to the atomic spacing
a)

The kinetic energy gained is eV=p22meeV=\dfrac{p^{2}}{2m_{e}}, so p=2meeVp=\sqrt{2m_{e}eV} and λ=hp\lambda=\dfrac{h}{p}. Numerically: p=2×9.11×10−31×1.60×10−19×54=3.97×10−24p=\sqrt{2\times 9.11\times 10^{-31}\times 1.60\times 10^{-19}\times 54}=3.97\times 10^{-24} kg·m/s and λ=1.67×10−10\lambda=1.67\times 10^{-10} m =0.167=0.167 nm.

b)

sin⁡θ=0.1670.215=0.777\sin\theta=\dfrac{0.167}{0.215}=0.777, so θ=51°\theta=51°. Davisson and Germer measured 50°50°: the agreement established the wave nature of the electron.

c)

λ∝1V\lambda\propto\dfrac{1}{\sqrt{V}}: to divide λ\lambda by 22, VV must be multiplied by 44, that is 216216 V. The classic mistake is to double the voltage.

d)

λ=h2mnE=6.63×10−342×1.675×10−27×0.025×1.60×10−19=1.81×10−10\lambda=\dfrac{h}{\sqrt{2m_{n}E}}=\dfrac{6.63\times 10^{-34}}{\sqrt{2\times 1.675\times 10^{-27}\times 0.025\times 1.60\times 10^{-19}}}=1.81\times 10^{-10} m =0.181=0.181 nm.

e)

Diffraction is pronounced only if the wavelength is of the same order as the spacing of the obstacles. The distances between atoms are a few tenths of a nanometre: that is precisely the wavelength of these electrons and neutrons, whereas visible light, from 400400 to 700700 nm, is a thousand times too large.

Part B: problems and reasoning (/50)

Exercise 6: X-rays: the Duane-Hunt limit and Moseley's law

In an X-ray tube, electrons accelerated through a voltage VV strike a metal anode. The emitted spectrum has a continuous background (bremsstrahlung, or braking radiation) that stops abruptly at a minimum wavelength, and lines characteristic of the metal. The Kα\alpha line approximately obeys Moseley's law: EKα≈10.2 (Z−1)2E_{K\alpha}\approx 10.2\,(Z-1)^{2} eV. Take hc=1240hc=1240 eV·nm. The diagram below shows the tube.

electronsX-raysV−+heated cathodeanode
  • a) For V=30.0V=30.0 kV, calculate the minimum wavelength of the continuous spectrum.
  • b) Why is there a minimum wavelength?
  • c) Calculate the energy of the Kα\alpha line of copper (Z=29Z=29), in keV.
  • d) Calculate its wavelength.
  • e) An unknown anode gives a Kα\alpha line at 0.1940.194 nm. Identify its atomic number.

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  • a) λmin=0.0413\lambda_{min}=0.0413 nm
  • b) A photon cannot exceed the energy eVeV
  • c) 8.008.00 keV
  • d) 0.1550.155 nm
  • e) Z=26Z=26, iron
a)

At best, an electron can give up all of its kinetic energy eV=30.0eV=30.0 keV to a single photon: λmin=hceV=124030 000=0.0413\lambda_{min}=\dfrac{hc}{eV}=\dfrac{1240}{30\,000}=0.0413 nm.

b)

Because energy is exchanged in photons: a shorter photon would have more energy than the electron that produces it, which conservation of energy forbids. Classical wave theory predicted no sharp cutoff; its existence is direct proof of quantization.

c)

E=10.2×282=8.00×103E=10.2\times 28^{2}=8.00\times 10^{3} eV =8.00=8.00 keV. It is the factor (Z−1)(Z-1), not ZZ, that appears: the electron dropping into the K shell “sees” the nucleus screened by the electron that remains there.

d)

λ=12408000=0.155\lambda=\dfrac{1240}{8000}=0.155 nm, the line used in laboratory diffractometers.

e)

E=12400.194=6.39×103E=\dfrac{1240}{0.194}=6.39\times 10^{3} eV, so (Z−1)2=639210.2=627(Z-1)^{2}=\dfrac{6392}{10.2}=627, Z−1=25.0Z-1=25.0 and Z=26Z=26: IRON. This is how Moseley ordered the elements by atomic number and predicted the missing elements of the periodic table.

0.050.100.15λ (nm)λminKαKβintensity

Exercise 7: The Franck-Hertz experiment

In a tube filled with mercury vapour, electrons are accelerated through an increasing voltage VV. The collected current rises, then drops suddenly at regularly spaced voltages: the peaks are separated by 4.94.9 V. At the same time, the vapour emits ultraviolet radiation.

Constants: h=6.63×10−34h=6.63\times 10^{-34} J·s, c=3.00×108c=3.00\times 10^{8} m/s, e=1.60×10−19e=1.60\times 10^{-19} C, me=9.11×10−31m_{e}=9.11\times 10^{-31} kg, hc=1240hc=1240 eV·nm.

51015voltage (V)anode current
  • a) What happens to an electron that reaches a kinetic energy of 4.94.9 eV?
  • b) Calculate the wavelength of the radiation emitted by the excited mercury atoms.
  • c) At what voltages do you expect the first three drops in current?
  • d) Calculate the speed of an electron with a kinetic energy of 4.94.9 eV.
  • e) How does this experiment, which uses no incident light, confirm the Bohr model?

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  • a) Inelastic collision: the atom is excited
  • b) λ=253\lambda=253 nm
  • c) 4.94.9 V, 9.89.8 V, 14.714.7 V
  • d) v=1.31×106v=1.31\times 10^{6} m/s
  • e) The atom is quantized, even without light
a)

As long as its energy stays below 4.94.9 eV, the electron bounces off the mercury atoms without losing energy (elastic collisions). As soon as it reaches 4.94.9 eV, it can give that energy to an atom by raising it to its first excited state: it loses almost all of its speed and no longer gets past the retarding grid, hence the drop in current.

b)

The excited atom returns to the ground state by emitting a photon of 4.94.9 eV: λ=12404.9=253\lambda=\dfrac{1240}{4.9}=253 nm, in the ultraviolet. This is indeed the observed line, the same one as in germicidal mercury lamps.

c)

An electron can excite an atom, be accelerated again, excite a second one, and so on: drops at 4.94.9 V, 9.89.8 V and 14.714.7 V. It is the constant spacing between the peaks, not the position of the first one (shifted in practice by the difference in the work functions of the electrodes), that measures the excitation energy.

d)

v=2Eme=2×4.9×1.60×10−199.11×10−31=1.31×106v=\sqrt{\dfrac{2E}{m_{e}}}=\sqrt{\dfrac{2\times 4.9\times 1.60\times 10^{-19}}{9.11\times 10^{-31}}}=1.31\times 10^{6} m/s.

e)

It shows that the atom accepts energy only in definite packets, even when that energy comes from a collision with an electron: quantization belongs to the ATOM, not only to light. And the emitted photon has exactly the energy measured electrically, which links the two methods.

Exercise 8: Five statements to correct

Each of the following statements is false, or false through a decisive detail. Choose the correct statement or give the requested value. Two marks each. Energy levels of hydrogen: En=−13.6n2E_{n}=-\dfrac{13.6}{n^{2}} eV.

  • a) “More intense light is made of more energetic photons.”
  • b) “In the hydrogen atom, the electron goes around a well-defined circular orbit, like a planet.”
  • c) “A hydrogen atom at rest in its ground state absorbs any photon with an energy between 10.210.2 and 13.613.6 eV.” To which level does a photon of 12.7512.75 eV raise the electron?
  • d) “Light is sometimes a wave and sometimes a particle, and it changes nature from one experiment to the next.”
  • e) “The absorption lines of a cold gas and the emission lines of the same hot gas fall at different wavelengths.”

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  • a) Intensity: number of photons
  • b) Probability of presence, no orbit
  • c) n=4n=4: only the exact gaps are absorbed
  • d) A single quantum object
  • e) Same wavelengths
a)

Intensity sets the NUMBER of photons per second; the energy of each photon depends only on its frequency, E=hfE=hf. A powerful red laser sends many photons of 1.91.9 eV, a weak ultraviolet lamp few photons of 44 eV.

b)

This is the Bohr model, useful for energies but superseded. Quantum mechanics gives no trajectory: it describes the electron by a wave whose square gives a PROBABILITY of presence, spread over “orbitals” with no sharp outline. The Bohr radius remains the most probable distance in the ground state.

c)

Absorption occurs only for energies equal to a gap between levels: 10.210.2 eV (1→21\rightarrow 2), 12.0912.09 eV (1→31\rightarrow 3), 12.7512.75 eV (1→41\rightarrow 4)... Above 13.613.6 eV, ionization accepts any energy. For 12.7512.75 eV: En=−13.6+12.75=−0.85E_{n}=-13.6+12.75=-0.85 eV, so n2=13.60.85=16n^{2}=\dfrac{13.6}{0.85}=16 and n=4n=4.

d)

Light does not change nature: it is a single quantum object, whose propagation is calculated like a wave and whose exchanges of energy take place in quanta. Sent photon by photon through Young's slits, it strikes the screen in point-like impacts that, in the long run, draw the interference pattern: the two aspects appear in the SAME experiment.

e)

They fall at the SAME wavelengths, because they correspond to the same gaps between energy levels: the photon absorbed to go up from E1E_{1} to E2E_{2} has the energy of the one emitted on the way back down. This is what makes it possible to identify the elements of a star from the dark lines of its spectrum.

Exercise 9: Problem: the shifted lines of a galaxy

The spectrum of a galaxy shows the Hα\alpha line of hydrogen at 658.4658.4 nm, whereas it is 656.3656.3 nm in the laboratory. For a speed vv small compared with cc, the Doppler effect gives Δλλ=vc\dfrac{\Delta\lambda}{\lambda}=\dfrac{v}{c}, with v>0v>0 for a receding source. Hubble's law: v=H0dv=H_{0}d with H0=70H_{0}=70 km/s per megaparsec (Mpc). c=3.00×105c=3.00\times 10^{5} km/s. The diagram below shows the two spectra around the line.

656.3 nm650655660665λ (nm)658.4 nmlaboratorygalaxy
  • a) Is the galaxy approaching or receding?
  • b) Calculate its radial speed, in km/s.
  • c) Calculate its distance, in Mpc.
  • d) Where does the Hβ\beta line (486.1486.1 nm in the laboratory) fall in this spectrum?
  • e) Why is the shifted line identified as Hα\alpha rather than as an unknown line?

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  • a) Receding (redshift)
  • b) v≈960v\approx 960 km/s
  • c) d≈13.7d\approx 13.7 Mpc
  • d) 487.7487.7 nm
  • e) Same factor for all lines
a)

The observed wavelength is LONGER: a redshift, so the galaxy is receding.

b)

v=cΔλλ=3.00×105×2.1656.3=9.6×102v=c\dfrac{\Delta\lambda}{\lambda}=3.00\times 10^{5}\times\dfrac{2.1}{656.3}=9.6\times 10^{2} km/s. We check that v≪cv\ll c (0.30.3 %): the non-relativistic formula is valid.

c)

d=vH0=96070=13.7d=\dfrac{v}{H_{0}}=\dfrac{960}{70}=13.7 Mpc, about 4545 million light-years.

d)

The RELATIVE shift is the same for all lines: λ=486.1×(1+2.1656.3)=487.7\lambda=486.1\times\left(1+\dfrac{2.1}{656.3}\right)=487.7 nm. The absolute shift, 1.61.6 nm, is smaller than that of Hα\alpha: this is the signature of a Doppler effect, and not of a calibration error, which would shift everything by the same amount.

e)

Because ALL the lines of hydrogen (Hα\alpha, Hβ\beta, Hγ\gamma...) are shifted by the same factor 1+vc1+\dfrac{v}{c}: the pattern of wavelength ratios set by the Bohr levels is preserved. We recognize the fingerprint of the element, then measure its shift.

Exercise 10: Problem: counting the photons of a barely visible star

A star at the limit of naked-eye visibility produces a light flux of 1.0×10−111.0\times 10^{-11} W/m² at ground level, which we assume to be concentrated at 550550 nm. The dilated pupil has a diameter of 7.07.0 mm. The eye integrates light over about 0.100.10 s.

Constants: h=6.63×10−34h=6.63\times 10^{-34} J·s, c=3.00×108c=3.00\times 10^{8} m/s, e=1.60×10−19e=1.60\times 10^{-19} C, me=9.11×10−31m_{e}=9.11\times 10^{-31} kg, hc=1240hc=1240 eV·nm. The diagram below shows the situation.

starflux at ground: 1.0 × 10⁻¹¹ W/m²λ = 550 nmretinapupil7.0 mm
  • a) Calculate the light power entering the pupil.
  • b) Calculate the energy of a 550550 nm photon.
  • c) How many photons enter the eye per second?
  • d) How many does it receive during its integration time?
  • e) A star is 100100 times fainter. How many of its photons enter the eye during the integration time? Why can the eye no longer see it, when a rod cell of the retina responds to a single photon?

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  • a) P=3.85×10−16P=3.85\times 10^{-16} W
  • b) E=3.62×10−19E=3.62\times 10^{-19} J
  • c) ≈1.06×103\approx 1.06\times 10^{3} photons/s
  • d) About 106106 photons
  • e) About one photon per integration time: coincidence threshold not reached
a)

Area of the pupil: π×(3.5×10−3)2=3.85×10−5\pi\times(3.5\times 10^{-3})^{2}=3.85\times 10^{-5} m². Power: P=1.0×10−11×3.85×10−5=3.85×10−16P=1.0\times 10^{-11}\times 3.85\times 10^{-5}=3.85\times 10^{-16} W. The RADIUS is half the diameter.

b)

E=hcλ=6.63×10−34×3.00×108550×10−9=3.62×10−19E=\dfrac{hc}{\lambda}=\dfrac{6.63\times 10^{-34}\times 3.00\times 10^{8}}{550\times 10^{-9}}=3.62\times 10^{-19} J.

c)

N=PE=3.85×10−163.62×10−19=1.06×103N=\dfrac{P}{E}=\dfrac{3.85\times 10^{-16}}{3.62\times 10^{-19}}=1.06\times 10^{3} photons/s.

d)

1.06×103×0.10≈1061.06\times 10^{3}\times 0.10\approx 106 photons, of which only a small fraction is absorbed by the rod cells.

e)

A hundred times less light means a hundred times fewer photons: 1.06×103100≈11\dfrac{1.06\times 10^{3}}{100}\approx 11 photons per second, one about every 9494 ms, so 11×0.10≈111\times 0.10\approx 1 photon per integration time. The brain reports a light only if several neighbouring rod cells are triggered within the same time interval: this is a filter against the “noise” of spontaneous triggering. With a single photon per integration time, most often lost before reaching a rod cell, the threshold is no longer crossed. Light remains granular at this level: a more sensitive detector, such as a photon-counting camera, would see it arrive grain by grain.

Part C: the classics (/50)

Exercise 11: The particle in a box: quantization from a standing wave

An electron is confined between two impenetrable walls a distance LL apart. Like a string fixed at both ends, its de Broglie wave must be STANDING with nodes at the walls: L=nλ2L=n\dfrac{\lambda}{2}, n=1,2,3…n=1,2,3\ldots Its energy, purely kinetic, is E=p22meE=\dfrac{p^{2}}{2m_{e}}.

Constants: h=6.63×10−34h=6.63\times 10^{-34} J·s, c=3.00×108c=3.00\times 10^{8} m/s, e=1.60×10−19e=1.60\times 10^{-19} C, me=9.11×10−31m_{e}=9.11\times 10^{-31} kg, hc=1240hc=1240 eV·nm.

n = 1n = 2n = 30L
  • a) Show that En=n2h28meL2E_{n}=\dfrac{n^{2}h^{2}}{8m_{e}L^{2}}, then calculate E1E_{1} in eV for L=1.00L=1.00 nm.
  • b) Calculate the energy of the photon emitted in the transition 2→12\rightarrow 1.
  • c) Calculate its wavelength, in nm.
  • d) In the hexatriene molecule, the 66 delocalized electrons behave like electrons in a box of L=0.73L=0.73 nm, two per level. Absorption raises an electron from level n=3n=3 to level n=4n=4. Calculate the absorbed wavelength.
  • e) Why can a confined electron never have zero energy?

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  • a) E1=0.377E_{1}=0.377 eV
  • b) ΔE=1.13\Delta E=1.13 eV
  • c) λ≈1.10×103\lambda\approx 1.10\times 10^{3} nm
  • d) λ≈250\lambda\approx 250 nm
  • e) Zero-point energy: n = 0 is forbidden
a)

λn=2Ln\lambda_{n}=\dfrac{2L}{n}, so pn=hλn=nh2Lp_{n}=\dfrac{h}{\lambda_{n}}=\dfrac{nh}{2L} and En=pn22me=n2h28meL2E_{n}=\dfrac{p_{n}^{2}}{2m_{e}}=\dfrac{n^{2}h^{2}}{8m_{e}L^{2}}. For L=1.00×10−9L=1.00\times 10^{-9} m: E1=(6.63×10−34)28×9.11×10−31×10−18=6.03×10−20E_{1}=\dfrac{(6.63\times 10^{-34})^{2}}{8\times 9.11\times 10^{-31}\times 10^{-18}}=6.03\times 10^{-20} J =0.377=0.377 eV. Quantization comes here from the standing-wave condition alone, with no additional postulate.

b)

E2−E1=(4−1)E1=3×0.377=1.13E_{2}-E_{1}=(4-1)E_{1}=3\times 0.377=1.13 eV.

c)

λ=12401.131=1.10×103\lambda=\dfrac{1240}{1.131}=1.10\times 10^{3} nm, in the near infrared.

d)

For L=0.73L=0.73 nm, E1=0.3770.732=0.707E_{1}=\dfrac{0.377}{0.73^{2}}=0.707 eV. The 66 electrons fill levels 11, 22 and 33; the transition 3→43\rightarrow 4 costs (16−9)E1=7×0.707=4.95(16-9)E_{1}=7\times 0.707=4.95 eV, that is λ=12404.95=250\lambda=\dfrac{1240}{4.95}=250 nm. The measured value is 258258 nm: a one-line model recovers the absorption of a real molecule to within 33 %. The longer the chain, the larger LL becomes and the more the absorbed colour slides toward the visible, hence the orange colour of carotene.

e)

The level n=0n=0 would give an infinite λ\lambda, a wave with no interior node that does not vanish at the walls: this is forbidden. The minimum energy is E1>0E_{1}>0, the “zero-point energy”, which grows as LL decreases. This is the uncertainty principle at work: to confine is to give momentum.

n = 1: E₁n = 2: 4E₁n = 3: 9E₁0L

Exercise 12: Why the Balmer lines of a star depend on its temperature

To produce a Balmer ABSORPTION line, a hydrogen atom must already be in the level n=2n=2, 10.210.2 eV above the ground state. At thermal equilibrium, the Boltzmann law gives N2N1=g2g1e−ΔE/(kT)\dfrac{N_{2}}{N_{1}}=\dfrac{g_{2}}{g_{1}}e^{-\Delta E/(kT)}, with gn=2n2g_{n}=2n^{2} states per level and k=8.62×10−5k=8.62\times 10^{-5} eV/K. The diagram below shows the levels involved.

n = 1n = 2n = 3n = ∞10.2 eVBalmerpopulation N₁population N₂
  • a) Calculate the ratio g2g1\dfrac{g_{2}}{g_{1}}.
  • b) Calculate kTkT at the surface of the Sun, 58005800 K.
  • c) Calculate N2N1\dfrac{N_{2}}{N_{1}} at 58005800 K (in ×10−9\times 10^{-9}).
  • d) Calculate N2N1\dfrac{N_{2}}{N_{1}} at 10 00010\,000 K (in ×10−5\times 10^{-5}).
  • e) Yet the Balmer lines are strongest in stars at around 10 00010\,000 K, and weaken in even hotter stars. Why?

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  • a) 44
  • b) kT=0.500kT=0.500 eV
  • c) 5.5×10−95.5\times 10^{-9}
  • d) 2.9×10−52.9\times 10^{-5}
  • e) Ionization of hydrogen above 10,000 K
a)

g2g1=2×42×1=4\dfrac{g_{2}}{g_{1}}=\dfrac{2\times 4}{2\times 1}=4.

b)

kT=8.62×10−5×5800=0.500kT=8.62\times 10^{-5}\times 5800=0.500 eV, twenty times less than the gap of 10.210.2 eV.

c)

N2N1=4 e−10.2/0.500=4 e−20.4=5.5×10−9\dfrac{N_{2}}{N_{1}}=4\,e^{-10.2/0.500}=4\,e^{-20.4}=5.5\times 10^{-9}. Not even one atom in a hundred million: the Sun nevertheless has visible Balmer lines, because the column of gas it passes through contains an enormous number of atoms.

d)

kT=0.862kT=0.862 eV and N2N1=4 e−11.83=2.9×10−5\dfrac{N_{2}}{N_{1}}=4\,e^{-11.83}=2.9\times 10^{-5}: five thousand times more than at 58005800 K, for a temperature barely doubled. The exponential makes the population of level 22 extraordinarily sensitive to temperature.

e)

Beyond roughly 10 00010\,000 K, hydrogen becomes massively IONIZED: the ionization energy is only 13.613.6 eV, and atoms that have lost their electron can no longer absorb a line. The population in level 22 therefore goes through a maximum. This is how Cecilia Payne showed, in 1925, that the differences between stellar spectra come from temperature and not from composition.

Exercise 13: Planck against Rayleigh-Jeans: the catastrophe in numbers

Planck's law gives the spectral radiance of a blackbody, BP=2hc2λ5⋅1ex−1B_{P}=\dfrac{2hc^{2}}{\lambda^{5}}\cdot\dfrac{1}{e^{x}-1} with x=hcλkTx=\dfrac{hc}{\lambda kT}. Classical physics predicted the Rayleigh-Jeans law, BRJ=2ckTλ4B_{RJ}=\dfrac{2ckT}{\lambda^{4}}. Constant: hck=1.439×10−2\dfrac{hc}{k}=1.439\times 10^{-2} m·K.

  • a) Show that BRJBP=ex−1x\dfrac{B_{RJ}}{B_{P}}=\dfrac{e^{x}-1}{x}.
  • b) For a body at 58005800 K, calculate xx at λ=500\lambda=500 nm.
  • c) Calculate the ratio BRJBP\dfrac{B_{RJ}}{B_{P}} at this wavelength.
  • d) Calculate the same ratio at λ=10\lambda=10 µm.
  • e) What happens to the Rayleigh-Jeans law as λ→0\lambda\to 0, and what did Planck's hypothesis change?

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  • a) ex−1x\dfrac{e^{x}-1}{x}
  • b) x≈4.96x\approx 4.96
  • c) About 28.628.6
  • d) About 1.141.14
  • e) Ultraviolet catastrophe avoided by quanta
a)

BRJBP=2ckTλ4⋅λ5(ex−1)2hc2=λkThc(ex−1)=ex−1x\dfrac{B_{RJ}}{B_{P}}=\dfrac{2ckT}{\lambda^{4}}\cdot\dfrac{\lambda^{5}(e^{x}-1)}{2hc^{2}}=\dfrac{\lambda kT}{hc}(e^{x}-1)=\dfrac{e^{x}-1}{x}.

b)

x=1.439×10−2500×10−9×5800=4.96x=\dfrac{1.439\times 10^{-2}}{500\times 10^{-9}\times 5800}=4.96.

c)

e4.96−14.96=28.6\dfrac{e^{4.96}-1}{4.96}=28.6: classical physics overestimates the visible radiation of the Sun by a factor of nearly thirty.

d)

x=1.439×10−210×10−6×5800=0.248x=\dfrac{1.439\times 10^{-2}}{10\times 10^{-6}\times 5800}=0.248 and e0.248−10.248=1.14\dfrac{e^{0.248}-1}{0.248}=1.14. At long wavelengths, when x≪1x\ll 1, ex−1≈xe^{x}-1\approx x and the two laws meet: classical theory was wrong only on the short-wavelength side.

e)

BRJB_{RJ} grows as 1λ4\dfrac{1}{\lambda^{4}} and diverges as λ→0\lambda\to 0: the total power would be infinite, the “ultraviolet catastrophe”. Planck assumes that the energy of a mode of frequency ff is exchanged only in quanta hfhf: at high frequencies, hf≫kThf\gg kT, these quanta are too costly to be excited, and the factor e−xe^{-x} shuts the spectrum off.

0.511.522.530.20.40.60.811.2at 500 nm: ratio 28.6Rayleigh-JeansPlanckλ (µm)relative radiance

Exercise 14: Laser cooling: stopping an atom photon by photon

A beam of sodium atoms (m=3.82×10−26m=3.82\times 10^{-26} kg) leaves an oven at 600600 m/s. A laser tuned to the 589589 nm line comes from the opposite direction. Each absorbed photon gives the atom a momentum hλ\dfrac{h}{\lambda} against its motion; the re-emitted photon leaves in a random direction, so its average contribution is zero. An atom absorbs at most 1.0×1071.0\times 10^{7} photons per second.

Constants: h=6.63×10−34h=6.63\times 10^{-34} J·s, c=3.00×108c=3.00\times 10^{8} m/s, e=1.60×10−19e=1.60\times 10^{-19} C, me=9.11×10−31m_{e}=9.11\times 10^{-31} kg, hc=1240hc=1240 eV·nm. The diagram below shows the situation.

ovensodium atom600 m/slaser589 nm photonsre-emitted photon:random direction
  • a) Calculate the change in the atom's speed at each absorption, in cm/s.
  • b) How many photons are needed to stop the atom?
  • c) How long does it take, at the maximum rate?
  • d) Calculate the corresponding deceleration, in multiples of g=9.8g=9.8 m/s².
  • e) Why must the laser frequency (or the tuning of the atom) be changed as the atom slows down, as in real experiments?

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  • a) Δv=2.95\Delta v=2.95 cm/s
  • b) N≈2.04×104N\approx 2.04\times 10^{4}
  • c) t≈2.0t\approx 2.0 ms
  • d) a≈3.0×104 ga\approx 3.0\times 10^{4}\,g
  • e) Track the Doppler shift
a)

Δv=hmλ=6.63×10−343.82×10−26×589×10−9=2.95×10−2\Delta v=\dfrac{h}{m\lambda}=\dfrac{6.63\times 10^{-34}}{3.82\times 10^{-26}\times 589\times 10^{-9}}=2.95\times 10^{-2} m/s =2.95=2.95 cm/s.

b)

N=6002.947×10−2=2.04×104N=\dfrac{600}{2.947\times 10^{-2}}=2.04\times 10^{4} photons.

c)

t=2.04×1041.0×107=2.0×10−3t=\dfrac{2.04\times 10^{4}}{1.0\times 10^{7}}=2.0\times 10^{-3} s: two milliseconds.

d)

a=Δv×107=2.95×105a=\Delta v\times 10^{7}=2.95\times 10^{5} m/s², that is 2.95×1059.8=3.0×104 g\dfrac{2.95\times 10^{5}}{9.8}=3.0\times 10^{4}\,g. Each kick is tiny, but the rate is enormous: the atom stops over a distance of v22a=0.61\dfrac{v^{2}}{2a}=0.61 m.

e)

Because of the Doppler effect: an atom rushing toward the laser sees the light at a higher frequency. The laser is tuned to be in resonance at 600600 m/s; as the atom slows down, it drops out of resonance, since the line is very narrow, and stops absorbing. The Doppler shift must be tracked throughout the braking.

Exercise 15: The natural width of a spectral line: energy-time uncertainty

A sodium atom stays on average τ=16\tau=16 ns in its excited state before emitting a photon of 589589 nm. The energy-time uncertainty relation, ΔE τ≈ℏ\Delta E\,\tau\approx\hbar, gives the line a natural width in frequency Δf=12πτ\Delta f=\dfrac{1}{2\pi\tau}. ℏ=1.055×10−34\hbar=1.055\times 10^{-34} J·s; e=1.60×10−19e=1.60\times 10^{-19} C; c=3.00×108c=3.00\times 10^{8} m/s. The diagram below, which is not to scale, shows the situation.

ground stateexcited statelifetime τ = 16 nsΔE589 nm photon
  • a) Calculate the uncertainty in the energy of the excited state, in eV (in ×10−8\times 10^{-8}).
  • b) Calculate the natural width Δf\Delta f, in MHz.
  • c) Calculate the frequency of the line (in ×1014\times 10^{14} Hz).
  • d) Calculate the relative width Δff\dfrac{\Delta f}{f} (in ×10−8\times 10^{-8}).
  • e) In a sodium vapour lamp at 500500 K, thermal motion broadens the line by Doppler effect by about 1.71.7 GHz. What can be concluded?

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  • a) ΔE≈4.1×10−8\Delta E\approx 4.1\times 10^{-8} eV
  • b) Δf≈9.9\Delta f\approx 9.9 MHz
  • c) f=5.09×1014f=5.09\times 10^{14} Hz
  • d) 1.95×10−81.95\times 10^{-8}
  • e) Doppler about 170 times wider
a)

ΔE≈ℏτ=1.055×10−3416×10−9=6.59×10−27\Delta E\approx\dfrac{\hbar}{\tau}=\dfrac{1.055\times 10^{-34}}{16\times 10^{-9}}=6.59\times 10^{-27} J, that is 6.59×10−271.60×10−19=4.1×10−8\dfrac{6.59\times 10^{-27}}{1.60\times 10^{-19}}=4.1\times 10^{-8} eV. A state that lasts only a finite time does not have a perfectly defined energy.

b)

Δf=12π×16×10−9=9.9×106\Delta f=\dfrac{1}{2\pi\times 16\times 10^{-9}}=9.9\times 10^{6} Hz =9.9=9.9 MHz. Consistency check: ΔEh=ℏ/τ2πℏ=12πτ\dfrac{\Delta E}{h}=\dfrac{\hbar/\tau}{2\pi\hbar}=\dfrac{1}{2\pi\tau}.

c)

f=cλ=3.00×108589×10−9=5.09×1014f=\dfrac{c}{\lambda}=\dfrac{3.00\times 10^{8}}{589\times 10^{-9}}=5.09\times 10^{14} Hz.

d)

Δff=9.95×1065.09×1014=1.95×10−8\dfrac{\Delta f}{f}=\dfrac{9.95\times 10^{6}}{5.09\times 10^{14}}=1.95\times 10^{-8}: the line is defined to two parts in a hundred million. This is what makes atomic clocks possible.

e)

The Doppler broadening, 1.7×1099.9×106≈170\dfrac{1.7\times 10^{9}}{9.9\times 10^{6}}\approx 170 times larger, completely dominates in a hot gas. To observe the natural width, the motion of the atoms must be suppressed, by cooling them with lasers or by using a beam perpendicular to the probe. The natural width is a fundamental limit, the Doppler width an experimental flaw.

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