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

Corrected exercises: modern physics (203-SN3-RE)

This is the corrected exercise set for Waves and Modern Physics, 203-SN3-RE (formerly 203-NYC), on modern physics. Part A follows the historical order: blackbody radiation with Wien's law and the Stefan-Boltzmann law, whose explanation forced Planck to quantize energy in 1900 (exercise 1); the energy of a photon and the graininess of light (exercise 2); the photoelectric effect and the argument that won Einstein his Nobel Prize (exercise 3); the hydrogen spectrum from the Bohr model (exercise 4); and the de Broglie wavelength, which extends wave-particle duality to matter (exercise 5). Part B moves up to exam level: the Compton effect, which makes the photon a true particle carrying momentum, followed by the uncertainty principle that fixes the size of the atom and keeps the electron out of the nucleus (exercise 6); carbon-14 dating (exercise 7); the mass defect, with the binding energy curve that explains fission and fusion in a single stroke (exercise 8); E=mc2E=mc^{2} applied to the Sun (exercise 9); and finally special relativity, with the atmospheric muons that should never reach us (exercise 10).

This set is written for CEGEP students in the Natural Science program (Sciences de la nature). This last chapter changes the rules of the game: energy is exchanged in packets, matter interferes, mass converts. The exercises remain computational, but every number carries an idea that started a revolution.

The reflex to keep throughout: the electron-volt is the currency of the chapter. Atomic energies are counted in eV, visible photons are worth between 1.8 and 3.1 eV, and converting to joules too early drowns the orders of magnitude. Stay in eV to the end, and go back to joules only for speeds and wavelengths. The classic trap of the chapter is dealt with in exercise 3: doubling the light intensity doubles the number of electrons emitted, never their energy.

10 corrected exercises • 100 points • 150 minutes

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Course recap

  • • Photon: E=hf=hcλE=hf=\frac{hc}{\lambda} with h=6.63×10−34h=6.63\times 10^{-34} J·s. Conversion: 1 eV =1.6×10−19=1.6\times 10^{-19} J. A handy shortcut: EE (in eV) ≈1240λ (nm)\approx\frac{1240}{\lambda\ \mathrm{(nm)}}.
  • • Photoelectric effect: Ephoton=W0+Ek,maxE_{photon}=W_{0}+E_{k,max}, where W0W_{0} is the work function of the metal. Threshold frequency: hf0=W0hf_{0}=W_{0}. Stopping potential: eVs=Ek,maxeV_{s}=E_{k,max}. The light intensity changes the NUMBER of electrons emitted, never their individual energy.
  • • Bohr atom (hydrogen): levels En=−13.6n2E_{n}=-\frac{13.6}{n^{2}} eV. A photon is emitted or absorbed when the electron jumps: Ephoton=∣Enf−Eni∣E_{photon}=|E_{n_{f}}-E_{n_{i}}|. Ionization energy from the ground state: 13.6 eV.
  • • Wave-particle duality: every particle of momentum p=mvp=mv has the de Broglie wavelength λ=hp\lambda=\frac{h}{p}.
  • • Radioactivity: N(t)=N0(12)t/T=N0e−λtN(t)=N_{0}\left(\frac{1}{2}\right)^{t/T}=N_{0}e^{-\lambda t} with the decay constant λ=ln⁡2T\lambda=\frac{\ln 2}{T} (TT: half-life). The activity (in becquerels) follows the same decay.
  • • Mass-energy equivalence: E=mc2E=mc^{2} with c=3.0×108c=3.0\times 10^{8} m/s. Electron mass: 9.11×10−319.11\times 10^{-31} kg.
  • • Blackbody radiation: Wien's law λmaxT=2.898×10−3\lambda_{max}T=2.898\times 10^{-3} m·K and the Stefan-Boltzmann law PA=σT4\frac{P}{A}=\sigma T^{4} with σ=5.67×10−8\sigma=5.67\times 10^{-8} W/(m²·K⁴). Doubling TT divides λmax\lambda_{max} by 2 and multiplies the radiated power by 16.
  • • Compton effect: Δλ=hmec(1−cos⁡θ)\Delta\lambda=\frac{h}{m_{e}c}(1-\cos\theta), with hmec=2.43\frac{h}{m_{e}c}=2.43 pm. The shift is ABSOLUTE, so it is negligible in visible light and measurable with X-rays. It proves that the photon carries p=hλp=\frac{h}{\lambda}.
  • • Uncertainty principle: Δx Δp≳ℏ\Delta x\,\Delta p\gtrsim\hbar with ℏ=1.055×10−34\hbar=1.055\times 10^{-34} J·s. Confining a particle costs it kinetic energy, which sets the size of the atom.
  • • Nucleus: mass defect Δm\Delta m and binding energy E=Δmc2E=\Delta m c^{2}, with 1 u =931.5=931.5 MeV/c2c^{2}. The binding energy per nucleon curve peaks at iron-56: fusion on the left, fission on the right, and both climb toward the peak.
  • • Special relativity: γ=11−v2/c2\gamma=\frac{1}{\sqrt{1-v^{2}/c^{2}}}, time dilation Δt=γΔtproper\Delta t=\gamma\Delta t_{proper}, length contraction L=LproperγL=\frac{L_{proper}}{\gamma}, energy E=γmc2E=\gamma mc^{2} and K=(γ−1)mc2K=(\gamma-1)mc^{2}. General relation: E2=(pc)2+(mc2)2E^{2}=(pc)^{2}+(mc^{2})^{2}, hence E=pcE=pc for the photon.

Part A: quanta, atoms and matter waves (/50)

Exercise 1: Blackbody radiation: Wien, Stefan and the birth of the quantum

Every hot body radiates. The maximum emission occurs at the wavelength given by Wien's law, λmaxT=2.898×10−3\lambda_{max}T=2.898\times 10^{-3} m·K, and the power radiated per unit area follows the Stefan-Boltzmann law, PA=σT4\frac{P}{A}=\sigma T^{4} with σ=5.67×10−8\sigma=5.67\times 10^{-8} W/(m²·K⁴). It was in trying to explain these two laws that Planck was forced, in 1900, to introduce the quantum. The diagram below shows the regions of the spectrum.

X-rayUVinfraredmicrowavesradio1 nm1 μm1 mm1 mwavelength λ (logarithmic scale)the regions of the electromagnetic spectrum
  • a) Calculate the wavelength of maximum emission of the Sun (surface at 5800 K) and of the human body (310 K). Place each in the spectrum and comment on the coincidence with the sensitivity of the eye.
  • b) The filament of an incandescent bulb reaches 2500 K. Calculate its maximum emission and explain why this type of bulb has such a poor luminous efficiency.
  • c) Estimate the NET power radiated by an unclothed person with a surface area of 1.8 m², at 306 K, in a room at 293 K. Comment on the order of magnitude.
  • d) Classical theory predicted that the radiated energy grows without limit as the wavelength decreases, which came to be called the ultraviolet catastrophe. Explain where this absurd prediction came from and how Planck's hypothesis removes it.
  • e) A star has a surface temperature twice that of the Sun. What happens to its maximum emission and to its power per square metre? Why is a red ember cooler than a white-hot piece of metal?

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  • a) 500500 nm for the Sun, 9.39.3 µm for the body: the eye adjusted to the solar maximum
  • b) 1.161.16 µm, in the infrared: luminous efficiency of about 5 %5\,\%
  • c) P=σA(T4−T04)≈140P=\sigma A(T^{4}-T_{0}^{4})\approx 140 W
  • d) High-frequency modes are FROZEN: the first quantum hfhf exceeds kTkT
  • e) λmax\lambda_{max} halved, power multiplied by 1616
a)

Sun: λmax=2.898×10−35800≈5.00×10−7\lambda_{max}=\frac{2.898\times 10^{-3}}{5800}\approx 5.00\times 10^{-7} m, that is 500 nm, right in the middle of the visible range, in the green. Human body: λmax=2.898×10−3310≈9.35×10−6\lambda_{max}=\frac{2.898\times 10^{-3}}{310}\approx 9.35\times 10^{-6} m, that is 9.3 μm, in the long-wave infrared, completely invisible to the eye but perfectly picked up by a thermal camera. The coincidence between the solar maximum and the peak sensitivity of the eye, around 555 nm, is of course no coincidence: the eye evolved under this light and adjusted to what was most abundant.

b)

λmax=2.898×10−32500≈1.16×10−6\lambda_{max}=\frac{2.898\times 10^{-3}}{2500}\approx 1.16\times 10^{-6} m, that is 1.16 μm: the maximum falls in the INFRARED, outside the visible range. An incandescent bulb therefore emits most of its radiation as invisible heat, and only the short-wavelength tail of its distribution reaches the visible; its luminous efficiency tops out around 5%. To do better, the temperature would have to go up, but tungsten melts at 3695 K: blackbody physics doomed the filament bulb long before regulations got involved.

c)

P=σA(T4−T04)=(5.67×10−8)(1.8)(3064−2934)≈1.4×102P=\sigma A(T^{4}-T_{0}^{4})=(5.67\times 10^{-8})(1.8)(306^{4}-293^{4})\approx 1.4\times 10^{2} W. About 140 W, more than the basal metabolic rate of an adult at rest, which explains why we cool down so quickly when unclothed, even in a room at 20 °C. The net power is proportional to the DIFFERENCE of the fourth powers, never to the difference of the temperatures: this is why a gap of only 13 degrees is enough to carry away that much energy. Clothing does not work by suppressing this radiation but by placing an intermediate surface in the way, colder on its outer side.

d)

Classical physics treated the radiation as a set of oscillation modes in a cavity, and the equipartition theorem gave each one the same average energy kTkT. But the number of modes grows without limit as the wavelength decreases: the total diverged, and one predicted that an open oven should emit a deadly burst of ultraviolet. Planck assumed that the energy of a mode of frequency ff can only be nhfnhf, an integer multiple. At high frequencies, the FIRST quantum hfhf is already much larger than the typical thermal energy kTkT: these modes simply cannot be excited, they stay frozen and stop contributing. The divergence disappears, and the calculated curve matches experiment exactly. Planck regarded this as a mathematical device; it was Einstein who, five years later, made it a physical reality with the photon.

e)

The wavelength of maximum emission is inversely proportional to TT: it is therefore halved, to 250 nm, in the ultraviolet, and the star looks blue-white since only the edge of its distribution is left to us. The power per square metre goes as T4T^{4}: it is multiplied by 24=162^{4}=16. The same law ranks the colours of heated objects: a red ember radiates around 1000 K, white-hot iron exceeds 1500 K, and its pale colour signals not a decorative nuance but a maximum emission shifted toward the blue and a power five times greater. In astronomy, the colour of a star is a thermometer.

500100015002000250030000.20.40.60.811.2visiblefilament, 2500 Kλmax = 1160 nmSun, 5800 Kλmax = 500 nmmaxima scaled to 1wavelength (nm)intensity (normalized)

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Exercise 2: The energy of a photon

Data: h=6.63×10−34h=6.63\times 10^{-34} J·s, c=3.0×108c=3.0\times 10^{8} m/s, 1 eV =1.6×10−19=1.6\times 10^{-19} J. The diagram below places these three kinds of radiation.

X-rayUVinfraredmicrowavesradio1 nm1 μm1 mm1 mwavelength λ (logarithmic scale)green light: 500 nmred laser: 650 nmFM station: 100 MHz
  • a) Calculate the energy of a photon of green light (500 nm), in joules and then in electron-volts.
  • b) Calculate the energy of a photon from an FM station at 100 MHz, in eV. Compare it with the visible photon and conclude about the perceptible graininess of the two kinds of radiation.
  • c) A red laser pointer (650 nm) emits 1.0 mW. How many photons does it emit per second?
  • d) Why can a radio antenna be described without difficulty with classical waves, whereas the interaction of X-rays with matter requires photons?

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  • a) E=hcλ≈4.0×10−19E=\dfrac{hc}{\lambda}\approx 4.0\times 10^{-19} J, that is ≈2.5\approx 2.5 eV
  • b) ≈4.1×10−7\approx 4.1\times 10^{-7} eV: six million times less
  • c) N=PE≈3.3×1015N=\dfrac{P}{E}\approx 3.3\times 10^{15} photons per second
  • d) It all comes down to the ratio between the quantum and the energies involved
a)

E=hcλ=(6.63×10−34)(3.0×108)500×10−9≈4.0×10−19E=\frac{hc}{\lambda}=\frac{(6.63\times 10^{-34})(3.0\times 10^{8})}{500\times 10^{-9}}\approx 4.0\times 10^{-19} J, that is 3.98×10−191.6×10−19≈2.5\frac{3.98\times 10^{-19}}{1.6\times 10^{-19}}\approx 2.5 eV. (Shortcut: 1240500=2.48\frac{1240}{500}=2.48 eV.) Visible photons all lie between 1.8 and 3.1 eV: the same scale as chemical bonds, which is why visible light drives photosynthesis and vision.

b)

E=hf=(6.63×10−34)(1.0×108)=6.6×10−26E=hf=(6.63\times 10^{-34})(1.0\times 10^{8})=6.6\times 10^{-26} J ≈4.1×10−7\approx 4.1\times 10^{-7} eV: six million times less than a visible photon. A radio receiver absorbs streams of billions of billions of photons: the grain is so fine that the energy looks perfectly continuous, just as a beach seen from afar looks smooth.

c)

Energy of a red photon: E=hcλ=1.989×10−25650×10−9≈3.1×10−19E=\frac{hc}{\lambda}=\frac{1.989\times 10^{-25}}{650\times 10^{-9}}\approx 3.1\times 10^{-19} J. Rate: N=PE=1.0×10−33.06×10−19≈3.3×1015N=\frac{P}{E}=\frac{1.0\times 10^{-3}}{3.06\times 10^{-19}}\approx 3.3\times 10^{15} photons per second: three million billion, for the most modest of laser pointers.

d)

Everything depends on the ratio between the quantum hfhf and the energies involved. In radio, hf≈10−7hf\approx 10^{-7} eV is tiny compared with everything: exchanges of billions of photons average out into a continuous wave, and the classical description is enough. An X-ray photon carries 10410^{4} to 10510^{5} eV: ONE photon is enough to ionize an atom, break a bond, or darken a grain of film: the interaction is an individual, discrete event that no continuous wave can describe. The classical-quantum boundary is not a question of size, but of relative graininess.

Exercise 3: The photoelectric effect: Einstein's argument

A metal has a work function W0=2.0W_{0}=2.0 eV. It is illuminated with violet light of 400 nm. The diagram below shows the setup.

microammeterpower supplycathodemetal: W₀ = 2.0 eVanodeviolet light: 400 nmA+COM+
  • a) Name two experimental observations of the photoelectric effect that the wave theory of light cannot explain, and show how the photon hypothesis explains them at a stroke.
  • b) Calculate the maximum kinetic energy of the ejected electrons, then the stopping potential.
  • c) Calculate the threshold wavelength of the metal. What happens if it is illuminated, even intensely, at 700 nm?
  • d) The intensity of the 400 nm light is doubled. What changes, and what does not? And what if we switch to 350 nm instead?

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  • a) The frequency threshold and the instantaneous emission: the exchange takes place in packets
  • b) E=3.1E=3.1 eV, Ek,max=1.1E_{k,max}=1.1 eV, Vs=1.1V_{s}=1.1 V
  • c) λ0=620\lambda_{0}=620 nm; at 700700 nm, no electron, whatever the intensity
  • d) Intensity and frequency act on two different knobs
a)

First, the existence of a frequency THRESHOLD: below f0f_{0}, no electron comes out, even under blinding light, whereas a wave should be able to accumulate the necessary energy by persisting. Second, the INSTANTANEOUS emission, even in very faint light, where a diluted wave should take minutes to charge up an electron. With the photon, everything becomes clear: the exchange takes place in packets hfhf, and an electron absorbs ONE photon; if hf<W0hf<W_{0}, the packet is too small and no accumulation is possible; if it is enough, ejection is immediate. The energy of light is not in its intensity but in its frequency: this is Einstein's reversal (1905).

b)

Photon of 400 nm: E=1240400=3.1E=\frac{1240}{400}=3.1 eV. Energy balance: Ek,max=E−W0=3.1−2.0=1.1E_{k,max}=E-W_{0}=3.1-2.0=1.1 eV. Stopping potential: Vs=Ek,maxe=1.1V_{s}=\frac{E_{k,max}}{e}=1.1 V: the voltage that cancels the current measures, directly in volts, the energy in eV.

c)

λ0=hcW0=12402.0=620\lambda_{0}=\frac{hc}{W_{0}}=\frac{1240}{2.0}=620 nm: an orange-red. At 700 nm, each photon carries only 1240700≈1.8\frac{1240}{700}\approx 1.8 eV <2.0<2.0 eV: NO electron comes out, whatever the intensity; multiplying photons that are too weak does not manufacture a photon that is strong enough.

d)

Doubling the intensity at 400 nm doubles the NUMBER of photons per second: twice as many electrons are ejected (double the current), but each with the same maximum energy of 1.1 eV: the stopping potential does not move. Switching to 350 nm changes the photon itself: E=1240350≈3.5E=\frac{1240}{350}\approx 3.5 eV, so Ek,max≈1.5E_{k,max}\approx 1.5 eV and Vs≈1.5V_{s}\approx 1.5 V, with a comparable current. Intensity and frequency act on two different knobs: this is exactly the particle signature.

12345678910−2.5−2−1.5−1−0.50.511.522.5f₀ = 4.8−W₀ = −2.0 eV400 nm: 1.1 eV350 nm: 1.5 eV700 nm: nothing emittedslope hfrequency f (× 10¹⁴ Hz)Ek max (eV)

Exercise 4: The hydrogen spectrum from the Bohr model

In the Bohr model, the energy levels of hydrogen are En=−13.6n2E_{n}=-\frac{13.6}{n^{2}} eV. The diagram below shows these levels, to scale.

n = 1n = 2n = 3n = 4, 5...E = 0ground stateemitted photonλ = ?energies to scale, in eV: En = −13.6 / n²
  • a) Calculate the energies of the first three levels. Why are these energies negative, and what does the zero mean?
  • b) Calculate the energy and the wavelength of the photon emitted in the transition from level 3 to level 2. What colour does it correspond to?
  • c) Calculate the ionization energy of the atom from its ground state and the maximum wavelength of a photon able to ionize it.
  • d) Explain why the emission spectrum of hydrogen is made of discrete lines and not a continuum, and why the ABSORPTION lines appear at exactly the same wavelengths.

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  • a) −13.6-13.6, −3.40-3.40 and −1.51-1.51 eV: the zero is the free electron at rest
  • b) 1.891.89 eV, that is ≈656\approx 656 nm: the red Hα\alpha line
  • c) 13.613.6 eV and λ≈91\lambda\approx 91 nm, in the far ultraviolet
  • d) Only the DIFFERENCES between levels exist, in emission and in absorption
a)

E1=−13.6E_{1}=-13.6 eV, E2=−13.64=−3.40E_{2}=-\frac{13.6}{4}=-3.40 eV, E3=−13.69≈−1.51E_{3}=-\frac{13.6}{9}\approx-1.51 eV. The zero is the reference: electron torn free, at rest, infinitely far from the proton. Bound energies are negative because energy MUST be supplied to free the electron: the minus sign measures the depth of the well.

b)

ΔE=E3−E2=−1.51−(−3.40)=1.89\Delta E=E_{3}-E_{2}=-1.51-(-3.40)=1.89 eV. Wavelength: λ=12401.89≈656\lambda=\frac{1240}{1.89}\approx 656 nm: the RED line of the Balmer series (Hα\alpha), the one that colours nebulae pink. A mental calculation recovers the colour of deep space: this is the triumph of the Bohr model (1913).

c)

From the ground state, 13.613.6 eV must be supplied. Maximum wavelength: λ=124013.6≈91\lambda=\frac{1240}{13.6}\approx 91 nm: far ultraviolet. Any shorter photon also ionizes (the surplus goes into the kinetic energy of the electron); any longer photon cannot, unless it finds the atom already excited.

d)

The electron does not have access to a continuum of energies: only the levels EnE_{n} exist, so only the DIFFERENCES Eni−EnfE_{n_{i}}-E_{n_{f}} can come out as photons: a comb of lines, the fingerprint of the element. In absorption, the mechanism works in reverse: the atom can swallow ONLY the photons whose energy matches an allowed jump exactly: same differences, same wavelengths, dark lines on a continuous background. This is how we read the composition of the Sun without going there: its absorption lines are the same as those of our hydrogen lamps.

n = 1-13.60 eVn = 2-3.40 eVn = 3-1.51 eVn = ∞0 eVn = 4, 5, ...LymanBalmerlevels crowd together as 1/n² toward ionization

Exercise 5: The de Broglie wavelength

In 1924, de Broglie postulated that every particle of momentum pp has a wavelength λ=hp\lambda=\frac{h}{p}. The diagram below shows the two situations.

cathodeanode100 Ve⁻electron acceleratedfrom rest40 m/sbaseballm = 145 g+
  • a) An electron is accelerated from rest through 100 V. Calculate its speed, its momentum and its de Broglie wavelength.
  • b) Calculate the de Broglie wavelength of a baseball (145 g) thrown at 40 m/s.
  • c) Compare the two results with characteristic sizes (atom: about 10−1010^{-10} m) and explain why the electron diffracts from a crystal whereas the ball will never diffract from anything.
  • d) Why does an electron microscope see details out of reach of the best optical microscope? Link the answer to the diffraction of the previous chapter.

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  • a) v≈5.9×106v\approx 5.9\times 10^{6} m/s and λ≈0.12\lambda\approx 0.12 nm
  • b) λ≈1.1×10−34\lambda\approx 1.1\times 10^{-34} m
  • c) The electron is at the atomic scale, the ball twenty-four orders of magnitude below
  • d) To see small, first illuminate short
a)

12mv2=eV\frac{1}{2}mv^{2}=eV gives v=2(1.6×10−19)(100)9.11×10−31≈5.9×106v=\sqrt{\frac{2(1.6\times 10^{-19})(100)}{9.11\times 10^{-31}}}\approx 5.9\times 10^{6} m/s. Momentum: p=mv≈(9.11×10−31)(5.93×106)≈5.4×10−24p=mv\approx(9.11\times 10^{-31})(5.93\times 10^{6})\approx 5.4\times 10^{-24} kg·m/s. Hence λ=hp=6.63×10−345.4×10−24≈1.2×10−10\lambda=\frac{h}{p}=\frac{6.63\times 10^{-34}}{5.4\times 10^{-24}}\approx 1.2\times 10^{-10} m: 0.12 nm.

b)

p=mv=(0.145)(40)=5.8p=mv=(0.145)(40)=5.8 kg·m/s, so λ=6.63×10−345.8≈1.1×10−34\lambda=\frac{6.63\times 10^{-34}}{5.8}\approx 1.1\times 10^{-34} m.

c)

The wavelength of the electron (100 V, barely a battery) falls RIGHT at the atomic scale: the planes of a crystal, spaced about 10−1010^{-10} m apart, form a natural diffraction grating for it: this is the Davisson-Germer experiment (1927), which confirmed de Broglie by observing electrons interfering like X-rays. The ball, for its part, is at 10−3410^{-34} m: twenty-four orders of magnitude below the size of an atom; no opening in the universe is fine enough to reveal its wave. The duality is universal in principle, invisible in practice as soon as hh is crushed by pp.

d)

Diffraction forbids resolving details smaller than about one wavelength: visible optics runs into the wall near 400 nm, a few thousand atoms. The electrons of part a), with 0.12 nm under a modest voltage (and far less still under 100 kV), lower this limit by several orders of magnitude: the electron microscope does not win through better lenses, it wins by changing the wave. To see small, first illuminate short.

Part B: exam level (/50)

Exercise 6: The Compton effect and the uncertainty principle

In 1923, Compton directed X-rays at graphite and found that the wavelength of the scattered radiation had INCREASED, by an amount that depends only on the angle: Δλ=hmec(1−cos⁡θ)\Delta\lambda=\frac{h}{m_{e}c}(1-\cos\theta). The incident X-ray has a wavelength of 71.0 pm. Parts d) and e) deal with the uncertainty principle, Δx Δp≳ℏ\Delta x\,\Delta p\gtrsim\hbar, with ℏ=1.055×10−34\hbar=1.055\times 10^{-34} J·s. The diagram below shows Compton's experiment.

graphiteX-ray: λ = 71.0 pmscattered photon: λ′θrecoil electron
  • a) Calculate the Compton wavelength hmec\frac{h}{m_{e}c}, then the shift for scattering at 90° and at 180°.
  • b) For scattering at 90°, calculate the energy of the incident photon and that of the scattered photon, in keV, then the kinetic energy given to the electron.
  • c) The shift does NOT depend on the incident wavelength. Calculate the relative shift for visible light at 500 nm and explain why the Compton effect requires X-rays.
  • d) What did this experiment definitively establish that the photoelectric effect had not yet shown?
  • e) An electron is confined in an atom, in one dimension of 1.0×10−101.0\times 10^{-10} m. Estimate its minimum momentum and the corresponding kinetic energy, in eV. Repeat the estimate for an electron one would try to lock inside a nucleus (10−1510^{-15} m), using E≈pcE\approx pc at this scale. What do you conclude?

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  • a) hmec=2.43\dfrac{h}{m_{e}c}=2.43 pm; 2.432.43 pm at 90°90° and 4.854.85 pm at 180°180°
  • b) 17.517.5 keV then 16.916.9 keV: the electron carries off ≈578\approx 578 eV
  • c) 3.4 %3.4\,\% for an X-ray against 5×10−65\times 10^{-6} in the visible
  • d) The photon has momentum: it is a true two-body collision
  • e) ≈3.8\approx 3.8 eV in the atom, but ≈200\approx 200 MeV in a nucleus: impossible
a)

hmec=6.63×10−34(9.11×10−31)(3.0×108)≈2.43×10−12\frac{h}{m_{e}c}=\frac{6.63\times 10^{-34}}{(9.11\times 10^{-31})(3.0\times 10^{8})}\approx 2.43\times 10^{-12} m, that is 2.43 pm. At 90°, cos⁡θ=0\cos\theta=0 and Δλ=2.43\Delta\lambda=2.43 pm. At 180°, backscattering, cos⁡θ=−1\cos\theta=-1 and Δλ=4.85\Delta\lambda=4.85 pm, the maximum possible. This is the signature of a collision: the photon gives up the most energy when it bounces straight back, exactly like a ball rebounding head-on.

b)

Incident photon: E=hcλ=(6.63×10−34)(3.0×108)71.0×10−12≈2.80×10−15E=\frac{hc}{\lambda}=\frac{(6.63\times 10^{-34})(3.0\times 10^{8})}{71.0\times 10^{-12}}\approx 2.80\times 10^{-15} J, that is 2.80×10−151.6×10−19≈17.5\frac{2.80\times 10^{-15}}{1.6\times 10^{-19}}\approx 17.5 keV. Scattered photon, with wavelength 71.0+2.43=73.471.0+2.43=73.4 pm: E′≈2.71×10−15E'\approx 2.71\times 10^{-15} J, that is 16.9 keV. By conservation of energy, the electron carries off the difference: E−E′≈5.8×102E-E'\approx 5.8\times 10^{2} eV, about 578 eV. Note how modest the transfer is, barely 3%: the photon bounces off a particle far more massive than it is, at least in terms of equivalent inertia.

c)

The shift is ABSOLUTE, always a few picometres, never proportional to λ\lambda. For an X-ray of 71 pm, it represents 2.4371.0≈3.4\frac{2.43}{71.0}\approx 3.4%, easily measurable. For visible light at 500 nm, it represents only 2.43×10−125.0×10−7≈4.9×10−6\frac{2.43\times 10^{-12}}{5.0\times 10^{-7}}\approx 4.9\times 10^{-6}, five millionths, undetectable with the means of the time and with an ordinary spectrometer today. This is why the effect stayed invisible as long as people worked only with visible light, and why X-rays were needed to reveal it: one needs a photon whose energy is comparable to the mass energy of the electron.

d)

The photoelectric effect established that light exchanges its energy in packets hfhf. It remained possible to save the idea of a wave by attributing the graininess to the metal rather than to the light. Compton closes that door: to account for the angular shift, one must apply conservation of MOMENTUM to the photon, with p=hλp=\frac{h}{\lambda}, exactly as in a two-body elastic collision in mechanics. The photon is therefore not just a grain of energy, it is a grain with momentum, which bounces, transfers and recoils. This is the point where the photon stops being a calculating convenience and becomes a particle, and Compton receives the Nobel Prize in 1927.

e)

In the atom: p≈ℏΔx=1.055×10−341.0×10−10≈1.06×10−24p\approx\frac{\hbar}{\Delta x}=\frac{1.055\times 10^{-34}}{1.0\times 10^{-10}}\approx 1.06\times 10^{-24} kg·m/s, hence Ek=p22me≈6.1×10−19E_{k}=\frac{p^{2}}{2m_{e}}\approx 6.1\times 10^{-19} J, about 3.8 eV. This is the same order of magnitude as the 13.6 eV that actually bind the electron: the uncertainty principle therefore explains the SIZE of the atom. Squeezing the electron closer to the nucleus would lower its potential energy, but at the price of a confinement kinetic energy that grows as 1Δx2\frac{1}{\Delta x^{2}}, hence faster: there is an equilibrium radius, and the atom does not collapse. In the nucleus: p≈1.055×10−341.0×10−15≈1.06×10−19p\approx\frac{1.055\times 10^{-34}}{1.0\times 10^{-15}}\approx 1.06\times 10^{-19} kg·m/s, and since this value is ultrarelativistic, E≈pc≈3.2×10−11E\approx pc\approx 3.2\times 10^{-11} J, nearly 200 MeV. Yet no nuclear force binds anything with such an energy, the binding energies per nucleon being of the order of 8 MeV. Conclusion: an electron can NOT reside in a nucleus, which definitively ruled out the model of nuclear electrons and, after the discovery of the neutron in 1932, imposed the nucleus made of protons and neutrons. The electrons of beta radioactivity do not pre-exist in the nucleus, they are created at the moment of the decay.

Exercise 7: Carbon-14 dating

Radioactive carbon-14 has a half-life of 5730 years. Living things maintain a constant proportion of carbon-14 as long as they exchange with the atmosphere; at death, the clock starts. The diagram below shows the situation.

atmosphere: CO₂ with ¹⁴Cliving: it exchanges,constant ¹⁴C fractionwood from the archaeological site:25% of the ¹⁴C of living wooddead: no more exchangecarbon-14: T½ = 5730 years
  • a) Explain the principle of dating: why is the proportion constant during life, and what happens afterwards?
  • b) A wood fragment from an archaeological site contains only 25% of the carbon-14 of living wood. Date it without a calculator.
  • c) Calculate the decay constant of carbon-14, then the exact age of a sample that retains 30% of it.
  • d) Explain why carbon-14 is useless for dating a dinosaur fossil (66 million years), and unreliable for an object 50 years old. What is the useful window of the method?
  • e) What would have to be used for the dinosaur? Give the principle behind the choice.

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  • a) Exchanges maintain the balance; at death, the clock starts
  • b) 25 %=(1/2)225\,\% = (1/2)^{2}, that is two half-lives: 11,46011{,}460 years
  • c) λ=ln⁡2T≈1.21×10−4\lambda=\dfrac{\ln 2}{T}\approx 1.21\times 10^{-4} yr⁻¹, and t≈9950t\approx 9950 years
  • d) Useful window from a few centuries to 50,00050{,}000 years
  • e) Choose your hourglass to match the duration to be measured
a)

Carbon-14 decays continuously, but living things renew it by breathing and eating: the balance between losses and supplies fixes the proportion. At death, exchanges stop while the losses continue: the proportion decays exponentially, and its present level measures the elapsed time. A dead organism is an hourglass that is never turned over again.

b)

25 %=14=(12)225\ \%=\frac{1}{4}=\left(\frac{1}{2}\right)^{2}: exactly TWO half-lives. Age: 2×5730=11,4602\times 5730=11{,}460 years: the end of the last glaciation. Each half-life halves what remains, whatever the starting point.

c)

λ=ln⁡2T=0.6935730≈1.21×10−4\lambda=\frac{\ln 2}{T}=\frac{0.693}{5730}\approx 1.21\times 10^{-4} yr−1^{-1}. Then N=N0e−λtN=N_{0}e^{-\lambda t} gives t=ln⁡(N0/N)λ=ln⁡(1/0.30)1.21×10−4=1.2041.21×10−4≈9950t=\frac{\ln(N_{0}/N)}{\lambda}=\frac{\ln(1/0.30)}{1.21\times 10^{-4}}=\frac{1.204}{1.21\times 10^{-4}}\approx 9950 years. Consistent: 30% lies between one half-life (50%) and two (25%), hence between 5730 and 11,460 years, closer to the second.

d)

At 66 million years, more than 11,000 half-lives have elapsed: the remaining fraction is (12)11,500\left(\frac{1}{2}\right)^{11{,}500}, zero to any physical precision: literally not one atom is left to count, and the slightest gram of modern contamination dominates the signal. At 50 years, conversely, only about 0.6% of the stock has decayed: the change is drowned in the uncertainties. The method is reliable, roughly, from a few centuries to 50,000 years: the clock must have run, but not run out.

e)

One needs an isotope whose half-life is comparable to the age being sought: for dinosaurs, geological pairs such as potassium-argon (T≈1.25T\approx 1.25 billion years) or uranium-lead, applied to the rocks that bracket the fossil. General rule: choose your hourglass to match the duration to be measured, just as you do not time a marathon with a three-minute egg timer.

500010000150002000025000300000.20.40.60.81T½25%: 11,460 years30%: 9950 yearsage (years)fraction of ¹⁴C remaining

Exercise 8: The nucleus: mass defect, fission and fusion

The mass of a nucleus is ALWAYS less than the sum of the masses of its nucleons taken separately; the difference, converted by E=mc2E=mc^{2}, is the energy that binds them. Take mp=1.00728m_{p}=1.00728 u, mn=1.00866m_{n}=1.00866 u, and the conversion 1 u =931.5=931.5 MeV/c2c^{2}. The helium-4 nucleus has a mass of 4.00151 u. The graph below gives the binding energy per nucleon of nuclei from carbon-12 to uranium-238.

4080120160200240246810iron-56: 8.8 MeVuranium-235number of nucleons Abinding energy/nucleon (MeV)
  • a) Calculate the mass defect of helium-4, its total binding energy and its binding energy PER NUCLEON.
  • b) The binding energy per nucleon curve peaks near 8.8 MeV around iron-56, then falls back. Explain why this shape makes TWO opposite sources of nuclear energy possible, and why iron is the end of the line.
  • c) A fission of uranium-235 releases about 200 MeV. Calculate the mass converted into energy, the fraction of the initial mass this represents, and the energy released per kilogram of uranium-235. Compare with coal, about 3×1073\times 10^{7} J/kg.
  • d) The deuterium-tritium fusion reaction releases 17.6 MeV for five nucleons. Calculate the energy per kilogram of mixture and compare with fission.
  • e) Estimate the Coulomb barrier between two light nuclei that must approach to 3×10−153\times 10^{-15} m, in keV. Compare it with the thermal energy kTkT at the core of the Sun (1.5×1071.5\times 10^{7} K, k=1.38×10−23k=1.38\times 10^{-23} J/K). How can fusion happen all the same?

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  • a) Δm=0.03037\Delta m=0.03037 u, E=28.3E=28.3 MeV, that is 7.077.07 MeV per nucleon
  • b) Fusion on the left, fission on the right: iron is at the top, hence the end of the line
  • c) ≈8.2×1013\approx 8.2\times 10^{13} J/kg, almost three million times coal
  • d) ≈3.4×1014\approx 3.4\times 10^{14} J/kg, four times fission
  • e) A barrier of 480480 keV against 1.31.3 keV thermal: tunnelling saves the day
a)

Sum of the free nucleons: 2(1.00728)+2(1.00866)=4.031882(1.00728)+2(1.00866)=4.03188 u. Mass defect: Δm=4.03188−4.00151=0.03037\Delta m=4.03188-4.00151=0.03037 u. Binding energy: E=(0.03037)(931.5)≈28.3E=(0.03037)(931.5)\approx 28.3 MeV, that is 28.34≈7.07\frac{28.3}{4}\approx 7.07 MeV per nucleon. In other words, assembling a helium nucleus releases 28 MeV, and the same amount would have to be supplied to take it apart. Relative to the total, the defect represents only 0.75% of the mass: the mass of an object is not the sum of the masses of its parts, it includes the binding energy, counted negatively.

b)

A nucleus to the LEFT of the maximum can gain binding energy per nucleon by fusing with another: it moves toward the peak, and the excess is released. A nucleus to the RIGHT gains instead by splitting in two pieces closer to iron: this is fission. The two processes therefore go in the same direction, that of the climb toward the maximum, but start from opposite sides. Iron-56, at the top, is the most tightly bound nucleus there is: neither fusing it nor splitting it yields anything, one must on the contrary pay in both cases. This is why a massive star, which makes heavier and heavier elements through successive fusions, stops dead when its core becomes iron: the energy source that held it up against its own gravity goes out, and the collapse that follows produces a supernova. All the elements heavier than iron were, moreover, forged in these cataclysms, against the energy current.

c)

Δm=200931.5≈0.215\Delta m=\frac{200}{931.5}\approx 0.215 u out of the 235 at the start, about 0.09% of the mass. Number of nuclei in one kilogram: 1000235×6.022×1023≈2.56×1024\frac{1000}{235}\times 6.022\times 10^{23}\approx 2.56\times 10^{24}. Total energy: (2.56×1024)(200×106)(1.6×10−19)≈8.2×1013(2.56\times 10^{24})(200\times 10^{6})(1.6\times 10^{-19})\approx 8.2\times 10^{13} J/kg. Coal provides 3×1073\times 10^{7} J/kg: the ratio is of the order of 2.7×1062.7\times 10^{6}, almost three million. One kilogram of uranium replaces about 2700 tonnes of coal, and this disproportion rests entirely on the fact that nuclear energies are counted in MeV whereas chemical energies are counted in eV.

d)

10005×6.022×1023≈1.20×1026\frac{1000}{5}\times 6.022\times 10^{23}\approx 1.20\times 10^{26} reactions per kilogram, each at 17.6 MeV: (1.20×1026)(17.6×106)(1.6×10−19)≈3.4×1014(1.20\times 10^{26})(17.6\times 10^{6})(1.6\times 10^{-19})\approx 3.4\times 10^{14} J/kg, about FOUR times the fission. The reason can be read directly on the curve of part b): fission gains 200236≈0.85\frac{200}{236}\approx 0.85 MeV per nucleon, D-T fusion gains 17.65≈3.5\frac{17.6}{5}\approx 3.5 MeV, four times more, because the slope of the curve is much steeper on the side of the light nuclei.

e)

U=ke2r=(9.0×109)(1.6×10−19)23.0×10−15≈7.7×10−14U=\frac{ke^{2}}{r}=\frac{(9.0\times 10^{9})(1.6\times 10^{-19})^{2}}{3.0\times 10^{-15}}\approx 7.7\times 10^{-14} J, about 480 keV. Thermal energy at the core of the Sun: kT=(1.38×10−23)(1.5×107)≈2.1×10−16kT=(1.38\times 10^{-23})(1.5\times 10^{7})\approx 2.1\times 10^{-16} J, only 1.3 keV: the barrier is nearly FOUR HUNDRED times too high. Classically, the Sun should not shine. Two quantum and statistical effects save the day. First, the Maxwell-Boltzmann distribution has a tail: a tiny but non-zero fraction of the nuclei moves much faster than the average. Next, and above all, TUNNELLING lets a nucleus cross the barrier without having the energy to climb over it, with a minuscule probability which, multiplied by the colossal number of nuclei and by the billions of years available, is more than enough. This improbability is, incidentally, humanity's good fortune: if fusion were easy, the Sun would have burned all its hydrogen in a few million years instead of ten billion.

4080120160200240246810iron-56: most tightly bound⁴He: 7.07fusion:going upfission: going up toward ironnumber of nucleons Abinding energy/nucleon (MeV)

Exercise 9: E = mc²: the Sun losing weight

The Sun radiates a power of 3.8×10263.8\times 10^{26} W. Its mass is 2.0×10302.0\times 10^{30} kg and its age about 4.5 billion years (1 year ≈3.16×107\approx 3.16\times 10^{7} s).

  • a) State what E=mc2E=mc^{2} means physically, and why the factor c2c^{2} makes the equivalence so spectacular.
  • b) Calculate the mass that the Sun converts into radiation every second.
  • c) Calculate the total mass radiated since its birth and the fraction of its mass this represents. Has the Sun noticeably lost weight?
  • d) A uranium fission releases about 200 MeV, a chemical combustion a few eV per molecule. Estimate the ratio and explain, using the vocabulary of the chapter, where the enormous energy density of nuclear power comes from.

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  • a) Mass and energy are two faces of one quantity, at the rate c2c^{2}
  • b) Pc2≈4.2×109\dfrac{P}{c^{2}}\approx 4.2\times 10^{9} kg/s
  • c) ≈6.0×1026\approx 6.0\times 10^{26} kg, that is 3.0×10−43.0\times 10^{-4} of its mass
  • d) 5×1075\times 10^{7}: chemistry rearranges electrons, nuclear power the nucleus
a)

Mass and energy are two faces of the same quantity: all energy has a mass, all mass is condensed energy, at the exchange rate c2=9.0×1016c^{2}=9.0\times 10^{16} J/kg. This colossal factor explains the asymmetry of everyday life: enormous energies correspond to tiny masses, which is why nobody had noticed the equivalence before 1905.

b)

ΔmΔt=Pc2=3.8×10269.0×1016≈4.2×109\frac{\Delta m}{\Delta t}=\frac{P}{c^{2}}=\frac{3.8\times 10^{26}}{9.0\times 10^{16}}\approx 4.2\times 10^{9} kg/s: more than four million tonnes per second, converted into light by the fusion of hydrogen into helium.

c)

Duration: 4.5×109×3.16×107≈1.4×10174.5\times 10^{9}\times 3.16\times 10^{7}\approx 1.4\times 10^{17} s. Mass radiated: (4.22×109)(1.42×1017)≈6.0×1026(4.22\times 10^{9})(1.42\times 10^{17})\approx 6.0\times 10^{26} kg. Fraction: 6.0×10262.0×1030=3.0×10−4\frac{6.0\times 10^{26}}{2.0\times 10^{30}}=3.0\times 10^{-4}: three hundredths of a percent in four and a half billion years. The most extreme regime in the universe costs the Sun almost nothing: there, in a single number, is the power of the exchange rate c2c^{2}.

d)

200×106 eV4 eV≈5×107\frac{200\times 10^{6}\ \mathrm{eV}}{4\ \mathrm{eV}}\approx 5\times 10^{7}: nuclear power releases tens of millions of times more energy per reaction than chemistry. The reason lies in the scales of the chapter: chemistry rearranges the ELECTRONS, bound by a few eV; nuclear power rearranges the NUCLEUS, whose bonds are counted in MeV, and the corresponding mass difference, about one thousandth of the mass of the nucleus, leaves as energy through E=mc2E=mc^{2}. One gram of nuclear fuel is thus worth tonnes of chemical fuel: same equation, upper storey of the atomic edifice.

Exercise 10: Special relativity: dilation, contraction and energy

Einstein's two postulates (1905) are that the laws of physics are the same in all inertial frames, and that the speed of light in them is always cc. From them follow the factor γ=11−v2c2\gamma=\frac{1}{\sqrt{1-\frac{v^{2}}{c^{2}}}}, time dilation Δt=γΔtproper\Delta t=\gamma\Delta t_{proper}, length contraction L=LproperγL=\frac{L_{proper}}{\gamma} and the energy E=γmc2E=\gamma mc^{2}. The mass energy of the electron is 0.511 MeV. The diagram below shows the situation.

detectormuoncreated by a cosmic rayv = 0.998c10.0 kmproper mean lifetime:2.2 μs
  • a) Calculate γ\gamma for v=0.60cv=0.60c, 0.90c0.90c and 0.99c0.99c. What do you notice about its growth?
  • b) A muon created at an altitude of 10.0 km travels at 0.998c0.998c and decays on average after 2.2 μs in its own frame. Calculate the distance it would travel without relativity, then the distance actually travelled. Repeat the reasoning IN the muon's frame and check that the two agree.
  • c) An electron is accelerated to 0.99c0.99c. Calculate its total energy and its kinetic energy, and compare the latter with the classical value 12mv2\frac{1}{2}mv^{2}.
  • d) Why can no massive object reach cc? Answer from the expression of the energy.
  • e) The general relation is written E2=(pc)2+(mc2)2E^{2}=(pc)^{2}+(mc^{2})^{2}. Check that it gives back E=mc2E=mc^{2} at rest, then apply it to the photon, whose mass is zero. What is the link with the de Broglie relation and with the Compton effect?

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  • a) 1.251.25, 2.292.29 and 7.097.09: γ\gamma explodes in the last few per cent
  • b) 659659 m without relativity against 10.410.4 km with; or 632632 m contracted as seen from the muon
  • c) E=3.62E=3.62 MeV, K=3.11K=3.11 MeV against 0.2500.250 MeV classically
  • d) γ→∞\gamma\to\infty as v→cv\to c: it would take an infinite energy
  • e) For the photon, E=pcE=pc gives p=hλp=\dfrac{h}{\lambda}: de Broglie and Compton united
a)

γ(0.60c)=11−0.36=10.80=1.25\gamma(0.60c)=\frac{1}{\sqrt{1-0.36}}=\frac{1}{0.80}=1.25; γ(0.90c)=10.19≈2.29\gamma(0.90c)=\frac{1}{\sqrt{0.19}}\approx 2.29; γ(0.99c)=10.0199≈7.09\gamma(0.99c)=\frac{1}{\sqrt{0.0199}}\approx 7.09. The growth is not steady: γ\gamma stays close to 1 over almost the whole range, then explodes in the last few per cent. At 60% of the speed of light, the effects do not exceed 25%, which explains why they stayed invisible through three centuries of mechanics.

b)

γ=11−0.9982≈15.8\gamma=\frac{1}{\sqrt{1-0.998^{2}}}\approx 15.8. Without relativity, the muon would travel d=vt=(0.998)(3.0×108)(2.2×10−6)≈659d=vt=(0.998)(3.0\times 10^{8})(2.2\times 10^{-6})\approx 659 m: it would cover only one fifteenth of the trip and practically no muon would reach the ground. With time dilation, its lifetime measured FROM THE GROUND is γ(2.2 μs)≈34.8\gamma(2.2\ \mu\text{s})\approx 34.8 μs, and the distance travelled is ≈1.04×104\approx 1.04\times 10^{4} m, more than 10 km: the muons arrive in abundance, which is indeed measured at sea level. In the frame of the MUON, nothing is dilated, its life does last 2.2 μs; but it is the atmosphere that rushes past, and its thickness is CONTRACTED: 10,00015.8≈632\frac{10{,}000}{15.8}\approx 632 m, which it crosses in 6320.998×3.0×108≈2.1\frac{632}{0.998\times 3.0\times 10^{8}}\approx 2.1 μs, roughly one lifetime. The two descriptions, one in dilated time, the other in contracted length, are incompatible in appearance and yet give exactly the same observable prediction. This is the heart of relativity: what is conserved is neither the duration nor the length, but the agreement on the FACTS.

c)

E=γmc2=(7.089)(0.511)≈3.62E=\gamma mc^{2}=(7.089)(0.511)\approx 3.62 MeV. Kinetic energy: K=(γ−1)mc2=(6.089)(0.511)≈3.11K=(\gamma-1)mc^{2}=(6.089)(0.511)\approx 3.11 MeV. The classical formula would give 12mv2=12(0.511)(0.99)2≈0.250\frac{1}{2}mv^{2}=\frac{1}{2}(0.511)(0.99)^{2}\approx 0.250 MeV, twelve times less. At this speed, Newtonian mechanics is not off by a little, it is off by an order of magnitude, which is why every particle accelerator is designed from end to end on the relativistic formulas.

d)

E=γmc2E=\gamma mc^{2} and γ→∞\gamma\to\infty as v→cv\to c: reaching exactly cc would require an INFINITE energy for any non-zero mass. No matter how much power is invested, one only nibbles at the decimals: at the Large Hadron Collider, protons reach 0.999999991c0.999999991c, with γ≈7500\gamma\approx 7500, and most of the energy supplied no longer serves to accelerate them but to increase their inertia. The speed of light is not a speed limit in the sense of a rule that could be broken: it is an asymptote built into the structure of spacetime.

e)

At rest, p=0p=0 and the relation gives E2=(mc2)2E^{2}=(mc^{2})^{2}, hence E=mc2E=mc^{2}: the mass energy is recovered as a special case. For a photon, m=0m=0, which leaves E=pcE=pc, that is p=Ec=hfc=hλp=\frac{E}{c}=\frac{hf}{c}=\frac{h}{\lambda}: the momentum of the photon, postulated by de Broglie and verified by Compton, comes straight out of relativity, with no additional assumption. The loop is closed: it is the same relation p=hλp=\frac{h}{\lambda} that describes matter as a wave in de Broglie and light as a particle in Compton. It also explains how the photon can carry momentum without having any mass at all, which makes radiation pressure, solar sails and laser cooling of atoms possible.

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